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We are delighted to announce the inaugural Global FUTR Lab in FutureEverything’s 20th year. We have partnered with the British Council’s Creative Economy team to select 10 of the world’s most innovative, interesting and irrepressible young creatives to take part in the festival and showcase their work.
Through a competitive application process, we are thrilled to welcome ten international innovators from Japan, Pakistan, South Korea, Nigeria, Ukraine, UAE and the UK to take part in FutureEverything’s festival programme, bringing a wealth of interdisciplinary approaches across art, technology, and innovation.
The ten participants will join the festival for an exclusive 5 day process, beginning with a two day lab and design sprint, facilitated by researchers from Strange Telemetry, using Manchester as inspiration. They will move past the ‘creative cities’ narrative to explore how industrial and cultural heritage influences their own practice.
The programme will form part of a larger discussion around critical approaches to innovation, seeking to move beyond assumed ideas on the value of ‘disruption’ to a richer understanding of the existing socio-technical systems and challenges which young entrepreneurs have to grapple with around the globe.
The 2015 Global FUTR Lab Participants
From Nigeria, Adebayo Adegbembo’s collection of interactive African culture teaching apps and videos – Asa (meaning culture in Yoruba) – aims to preserve, educate and creatively deliver the rich heritage of the continent.
Looking at the importance of sharing community data, Areeb Karman’s Noustix project (Pakistan) is a unique platform for collecting, visualizing, and analyzing “Geo-Spatial-Temporal” data, which can be used to plot maps used by the community and elsewhere.
Also using data in their work, Ukraine’s Ivan Pasichnyk project Ecoisme aims to create better relationships between customers and energy providers, using sensor data and cloud technologies to encourage better attitudes and tools for sustainable energy.
Chronically Driven (CD) is a digital social innovation, created by Bhavani Esapathi (UK), which is aimed at bringing awareness of chronically debilitating illnesses to the forefront of social media. Using social media and online platforms to create better community support and communicate with the wider public, CD works to encourage positive social impact on the medical community, leading to increasing medical support.
From the UK, creative technologist Dan Williams’ Postcards from a Supply Chain is a necessary exploration of the manufacturing, production routess and supply chains of the world’s personal electronics. Told in first person, Dan’s project is a result of the Unknown Fields exploration which saw a team of writers, researchers and technologists embark on a cargo ship through one of China’s major shipping channels.
From the United Arab Emirates the interdisciplinary designer, and a maker Salem Al-Mansoori will be presenting his explorations into social cartography and online wayfinding systems. Salem’s passion is generative, data-driven, narrative-based works, with a focus on creating digital fabrication to data visualization to algorithm-based visual art installations.
Often the way we can feel out systems, or understand their limits, is through physically playing with them. Korea’s Hee Eun Kim has developed an interactive installation, Net Disruption, to facilitate a new approach to our experience and perception of network space through a series of transformative strings.
With play and curiosity and the heart of the organisation, Leila Johnston (UK), is bringing her multidisciplinary art and research Hack Circus to Global FUTR lab. Part magazine, part event, part experimentation, Hack Circus works at breaking down boundaries between performers and audience, artists and technologists to disrupt assumptions about identity.
Exploring new ways to use exhibition spaces, Japan’s Nozomi Matsuyama has developed a collaborative approach to curation, Sckell Building Exhibition. Using three floors of a building as series of interfaces to bring interdisciplinary practitioners and disciplines together, this project causes an exhibition to function as a crossing point of daily life and images
Indonesia’s Venzha Christ is currently looking to change the innovation and making landscape of South East Asia, using his time with the Global FUTR lab to develop one of his ongoing proposals, including creating the first FabLab in South East Asia. His other project, Transformaking 2015, is a push to induct the first International Summit on Critical and Transformative Making in Indonesia, 2015.


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Health Services are provided for all Southwest Christian students during the school day by a registered nurse (RN) or a licensed practical nurse (LPN).
Please fill out the medical forms located on our Forms page before the start of each school year. Printed forms are to be returned to the receptionist two weeks before school starts.
- First Aid
- Immunization monitoring
- Prescribed health procedures
- Surveillance of communicative diseases
- Managing individualized health plans for student with health concerns
- Maintaining health records
- Special education team member
- Crisis team planning and response
- Vision and hearing screenings are available upon request
To Send or Not to Send?
In order to maintain the health of the Southwest Christian community, we ask our parents to be diligent about keeping their child home from school if certain symptoms are present. A student should be excluded from school with any of the following conditions:
- Fever of 100 or more – Student must stay home for 24 hours after the temperature returns to normal
- Vomiting and diarrhea – Student must stay home until 24 hours after the last episode
Any undiagnosed rash – Student must see a physician before admittance to school
- Chicken pox – Student may return to school after the last pox has scabbed over, usually 7–10 days
- Any uncontrolled cough
- Influenza – Student may return if he/she is feeling better (anywhere from 2–7 days)
- Impetigo – Student may return to school 24 hours after treatment
- Lice – Student may return after treatment
- Pink eye – Student may return after treatment if there is no pus-like drainage
- Ringworm – Student may return 24 hours after treatment
- Scabies – Student may return 24 hours after treatment
- Strep throat – Student may return 24 hours after first antibiotic treatment
- Pinworm – Student may return after treatment
- Hand, foot, & mouth disease – Student may return 24 hours after temperature returns to normal. If you have any questions regarding sending your child to school, please contact the Southwest Christian health office.
No Shots, No School. Starting in the 2001 school year, Independent School District 112 began enforcing the “No Shots, No School” policy. Students who are not up to date on their immunizations will not be allowed to start school until they receive the proper booster shots and provide the school with documentation of these vaccines. Parents may choose to decline immunizations for their child, for medical reasons or conscientiously held beliefs, by getting a legal exemption from Minnesota school law.
If you have any questions regarding your child’s vaccines, please contact your physician or a Southwest Christian school nurse.
- Any student that will take a non-prescription medication during school hours must have a Medication Authorization Form filled out and signed by the parent/guardian prior to medication dispensing. Be sure to include child’s name, name of medication, amount to be taken, and time to be given.
- Prescription medications need a physician’s signature prior to medication dispensing.
- All medications must be sent to school in the original pharmacy container with the student’s name printed on the label as well as the medication and dosage to be administered.
- If your child carries an inhaler/Epi-pen with him/her (in backpack, pocket, desk, or locker), a written permission form, including student, parent, and physician signature, must be kept on file in the health office.If there are any questions or concerns please contact the school nurse.

domain: medical


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The game is to have them running about with fire extinguishers whenever there is a flood, and all crowding to that side of the boat which is already nearly gunwale under. […] Cruel ages are put on their guard against Sentimentality, feckless and idle ones against Respectability, lecherous ones against Puritansm; and whenever all men are really hastening to be slaves or tyrants we make Liberalism the prime bogey.
But the greatest triumph of all is to elevate their horror of the Same Old Thing into a philosophy. […] And great work has already been done. Once they knew that some changes were for the better, and others for the worse, and others again indifferent. We have largely removed this knowledge. For the descriptive adjective ‘unchanged’ we have substituted the emotional adjective ‘stagnant’. We have trained them to think of the Future as a promised land which favoured heroes attain—not as something which everyone reaches at the rate of sixty minutes an hour, whatever he does, whoever he is.
– C. S. Lewis, The Screwtape Letters (1942)

domain: literature


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The opening kick-off event for the Hollywood SAG Film Society season is only two weeks away. It's not too late to join at last year's membership fee. Space is limited. Hurry and join your fellow SAG members today and we'll see you at the movies!
5757 Wilshire Boulevard, 7th Floor
Los Angeles, California

domain: hobby


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The Medical College of Wisconsin (MCW) has received a five year, $1.5 million grant from the National Institute of Health’s National Institute of Allergy and Infectious Diseases to study the pathogenesis of Pseudomonas aeruginosa, a bacterium that is intrinsically resistant to antimicrobials, and that is difficult to treat.
Dara Frank, PhD, professor of microbiology and molecular genetics and director of MCW’s Center for Infectious Disease Research, is the primary investigator of the grant. Jimmy Feix, PhD, professor of biophysics, is a co-investigator.
Pseudomonas aeruginosa has been linked to burn victims, immunocompromised patients, and individuals with cystic fibrosis. Colonization of organs such as the lungs or spread of the bacteria to the bloodstream, can result in a fatal infection. Toxins expressed by the bacteria make it particularly pathogenic.
In this study, Dr. Frank will study a toxin expressed by Pseudomonas aeruginosa called ExoU, which is correlated with poor outcomes in human infection. By studying ExoU and the system in which it is expressed, new insights about the pathogenic nature of the bacteria will be discovered, with the ultimate goal being to provide unique targets and biological tools to limit that pathogenicity—and improve outcomes in human infections.
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- Abby Thompson will appear in Milwaukee Rep Theater's production of A Christmas Carol
- St. Margaret Mary School to Donate 13,200 Pounds of Food
- Richard Kohlmann Named Beverage Manager at Western Racquet Club
- Area Students Perform in Miracle on 34th Street at Sunset Playhouse December 4th through December 31st
- Acclaimed actor Michael York to keynote amyloidosis event
- YOUNG WAUWATOSA RESIDENT APPEARS IN FIRST STAGE'S RUDOLPH THE RED-NOSED REINDEER
- Shop Small on Small Business Saturday
- Milwaukee/NARI Home Improvement Council Honors Barry Mandel With the “Building Milwaukee” Award
- Local Businesses Collect, Deliver More than 4,000 Pounds of Food to New Berlin Food Pantry
- TOP 10 THINGS YOU NEED TO KNOW WHEN BUYING A HOME

domain: biology


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Vegetarian Foods That Are Not Vegetarian
As followers of this blog probably already know, I am a Vegan. I don’t eat any animal products, nor do I have any oil in my diet. I don’t do this because I am overly sensitive to small, furry creatures, but rather for my health. Note: This does not mean you should send me a list of emails stating that this is a terrible diet and that I need to add fat so my brain functions. It works great! I was recently shocked to find out that some of our favorite foods do not comply with my eating choices. You might find this list a little disturbing once you read it, as well, but these are vegetarian foods that are not vegetarian.
When you grab a bag of sugar, most of the time the ingredient list will just list “sugar” as its sole ingredient. Amazingly, that’s not true. Sugar isn’t naturally white. It’s processed and turned white. Brown sugar and powdered sugar are processed, as well. So what are these companies using to create the white, sweet granules that we know and love? Natural Carbon. At least that’s the name they call it so that you don’t get sick while you’re eating your sweetened corn flakes. Natural carbon is ground up bone char from animals! Yum! Never fear, though. You can always use unrefined sugar or sugar-in-the-raw as a replacement from cow skeleton…
Do you like to eat candy? Everyone loves a piece of candy once in awhile. When I was a kid, they always told us to brush our teeth so they didn’t decay. Little did your parents know, the candy wasn’t the bad part of what was going into your mouth. It was the coloring. Next time you have a hankering for some candy, check to see if these words are used in the ingredients: Cochineal, Carminic acid or Carmine. If they are, congratulations! You’re eating beetles! Those ingredients are made from the female Dactylopius coccus costa, or cochineal insect. Many candies are also coated with shellac, a resin excreted by the lac bug, which is usually listed as ‘confectioner’s glaze’.
In the middle of summer, a nice and refreshing beer often hits the spot. That is until you realize that they like to strain the yeast with fish bladders! Isinglass is a membrane taken from the bladders of tropical fish and is used to filter cloudy yeast extracts out of many brands of beer and wine. Not all beers and wines use this, but you should be aware of the ones that do. They can fool you because they do not smell fishy.
Mmmm…Twinkies. You might think again when you consider that many store bought cake mixes and all Hostess Snacks – from HoHos to Fruit Pies to Ding Dongs – all contain Beef Fat. You know. It’s the stuff that you cut off your steak and throw away? Some of it makes it into your dessert. It can be deceptive because sometimes they disguise ‘beef fat’ with words like ‘lard’. However, no matter how you cut it, it’s that white, gelatinous suet that you would never eat if saw it on your New York strip steak.
How can orange juice contain animal products? It’s grown on a tree and squeezed into a glass! If you get your orange juice freshly squeezed, then there is nothing to worry about. It’s when we try to go that extra step for vitamins that we start seeing animal products in our morning juice. Look out for juices that are fortified with Vitamin D3. That’s a signal that they strained your juice with lanolin. Lanolin is the oil that comes off of sheep’s wool. Your taste buds are probably already getting excited! Also look out for Omega-3 additions. This nutrient is derived from fish oil and gelatin. Gelatin is the yummy by-product of pig skin and cow bones. You can also find it in Jello, marshmallows, ice cream and yogurt!

domain: food


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North coast of Lancashire, north of Blackpool and Preston. Includes Fleetwood and Poulton-le-Fylde, which are contiguous with Blackpool; the district is divided by the River Wyre. Also stretches to Garstang on the M6.
There is a vacancy in Rossall ward (also held by Labour). The Conservatives gained Bourne ward from Labour on 4 May.
Next local elections

domain: politics


- Motolotov cocktail thrown a Brooklyn mini-mart
- 3 Americans dead in shooting at Kabul hospital by Afghan guard
- Running on empty: EPA slashes biofuel goals because of ethanol shortage
- ‘Gay Jeans’ that fade into rainbow-colored denim created
- Divided court strikes down big porn award
- Jimmy Carter: Don’t hurt Russian people with sanctions
- Oldest ex-MLB player dies in Cuba, 2 days shy of 103rd birthday
- ‘Top Gun’ for drones: Squadrons of carrier-based killers have Navy’s approval
- Bill Clinton to endorse Charlie Rangel for re-election
- Pfc. Bradley Manning is now Pfc. Chelsea Manning: Court says so
By Andrew P. Napolitano
Obama's veil of secrecy is pierced
Topic - Marion Jones
Drug scandals have become even more prevalent in recent years and it is enough to make a cynic wonder about any significant athletic feat: clean or not clean?
Former track star Marion Jones is making a series of diplomatic visits to Serbia and Croatia this week on behalf of the U.S. State Department, an international opportunity for her to continue rehabilitating her tarnished image.
Former Olympic gold medal-winning sprinter Marion Jones has been cut by the WNBA's Tulsa Shock, bringing her future in basketball into question.
As her first season in the WNBA comes to a close, Marion Jones is pleased with her progress and committed to continuing her development.
Tiffany Jackson scored 17 points, former Olympic sprinter Marion Jones finished her rookie season with a career-high 14 points and the Tulsa Shock snapped a six-game losing streak Saturday night by beating the Chicago Sky 84-71.
Either Roger Clemens or Brian McNamee is lying, one of the charges against Marion Jones that resulted in a six-month prison sentence.
Marion Jones told us all about winning five golds in Sydney, but neglected to add the part about being juiced while she ran past everyone.
Jones said a big jump in muscle year-over-year — say 40 pounds — would be a "red light that something is not right."


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Yaaaay! It's here! The 24in48 Readathon! The goal this weekend is to read for 24 of the 48 hours between midnight Friday and midnight Sunday.
I'm not much of a night owl, so I've scheduled this post and will begin reading whenever I wake up Saturday. It's been a beast of a week, so hopefully I will actually sleep in a little bit. I'd like to read for at least 20 hours this weekend; 24 hours will be a stretch goal for me. :)
Here's my reading pile:
And I've got tons of galleys on my Kindle, too:
Plus, I keep forgetting and then remembering with delight that I have Patina on my Kindle, too. I've been saving it for this weekend, so that's one I'll tackle for sure!
I will NOT be reading all of these. I love to have lots of choices for Readathons, so I surround myself with great books. If I finish five books this weekend, I will be thrilled!
My husband C will be reading this weekend, too, although probably less diligently than I. He's got his stack ready to go. Lots of anthologies, which are great for finding new authors. He just finished a massive Stephen King reading project, so he's ready to discover some new fantasy and horror.
I'll post a couple of times throughout the weekend, but I'll probably make more frequent updates on Litsy and Instagram, so feel free to follow along! If you're doing the Readathon this weekend, let me know! I love the camaraderie of everyone reading together, even though we're not physically together!


Why the clamor in Albuquerque, New Mexico for Bernalillo County Commissioner Michael Wiener to resign? So he went to the Phillipines and unwittingly ended up being photographed there in the red light district. He went on his own dime and is unmarried.
As I see it, he's only guilty of being a white Republican male. I noticed no one at the Albuquerque Journal (which seems to be spearheading the drive for Wiener's removal) raised a peep when the homosexual group PFLAG recently said they were going to hold their own prom for high schoolers who share their unnatural orientation here. Apparently heterosexuality is wrong but sodomy is okay.
It is fascinating to watch this strange behavior from the same media which not so long ago excused Bill Clinton's adultery by claiming it was his own business. Liberals seem to view their hypocrisy as a moral privilege, I guess.
by © Clyde James Aragon
from "Full Frontal Stupidity" - http://fullfrontalstupidity.blogspot.com/
see more of him at http://www.zazzle.com/cja_the_humorist*


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AIJU is collaborating in the development of a new research and development project of CDTI, “Development of a biodegradable film with biopesticidal/repellent properties”, (File No.: IDI-20141480), led by the company, INDUSTRIAS PLÁSTICAS BAÑERES, S.A (INPLASBA).
The main objective of the project is to develop a biodegradable film capable of progressively releasing natural substances with biopesticidal and repellent properties, which would protect banana crops from various pests that attack the fruit, and that would not be a source of pollution for the environment or a risk to health of farmers or consumers.
Currently, the practice of bagging banana branches with a polyethylene film is performed to protect the banana fruit from the negative effects of the environment (burning by sun, excess humidity) and to help in the control of pests, insects and others, enabling harvesting cleaner fruit, of greater weight and in less time.
The main differences of the product to be developed in comparison with the current product are:
Start date: 1 June 2014

domain: agronomy


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Joule heating in high magnetic field pulsars
Key Words.:MHD - stars: neutron - stars: magnetic fields - pulsars: general
Aims:We study the efficiency of Joule heating in the crustal layers of young neutron stars.
Methods:The induction equation is solved numerically for a realistic crust model with a conductivity that depends on the density and temperature.
Results:We show that dissipation of the magnetic field is highly inhomogeneous in the crust with much faster dissipation in relatively low density layers. In young neutron stars, the rate of Joule heating in the crust can exceed the standard luminosity of non-magnetic stars and can even be comparable to the luminosity of magnetars.
Conclusions:The results of calculations are compared with the available observational data. We argued that the crustal field model can well account for the data on the surface temperature and magnetic field of young neutron stars.
The influence of the magnetic field on the thermal history of neutron stars is twofold. On one hand, the field changes the character of heat transport providing some anisotropy to kinetic processes. Such anisotropic transport can result in a characteristic temperature difference between the poles and equator caused by large-scale inhomogeneities of the magnetic field (see, e.g., Potekhin et al. 2003; Perez-Azorin et al. 2006). On the other hand, dissipation of the magnetic field provides an additional heating mechanism that can substantially alter the cooling evolution (Miralles et al. 1998). Even more or less standard for radiopulsars magnetic fields G can maintain the surface temperature as high as K for Myr which is substantially higher than predicted by various cooling models. A general relativistic treatment of Joule heating in neutron stars undertaken by Page et al. (2000) led to results very similar to those of Miralles et al. (1998) since, as it was argued by Konar (2002), general relativistic corrections do not significantly influence the magnetic field decay in neutron stars.
The internal magnetic fields in neutron stars, however, can be substantially stronger than the “standard” surface field of radiopulsars, and they can produce much more efficient heating. The nature of pulsar magnetism is still the subject of debate. One of the possibilities is associated with the turbulent dynamo action that can amplify the magnetic field during the first s of a neutron star’s life when the star is subject hydrodynamic instabilities (Thompson & Duncan 1993; Bonanno et al. 2003). Turbulent motion caused by instabilities in combination with rapid rotation that seems to be almost inevitable in protoneutron stars make a turbulent dynamo one of the most plausible mechanisms of pulsar magnetism. The characteristic feature of a turbulent dynamo in stars is that generation of the large-scale field is always accompanied by generation of small-scale fields that are approximately in equipartition with the turbulent motion. Therefore, if the field of pulsars is of dynamo origin, it should have a very complex geometry when dynamo action stops (see Urpin & Gil 2004, Bonanno et al. 2005, 2006). Magnetic fields of various scales will be frozen into the crust that begins to form soon after the end of the unstable stage and then will decay due to the finite crustal resistivity.
Miralles et al.(1998) have considered the effect of Joule heating in old neutron stars with an age yrs, when the surface temperature is low and dissipation of even standard pulsar magnetic fields can change the thermal evolution substantially. In this paper, we treat the effect of dissipation during the early evolution of neutron stars ( yrs), when neutron stars are much hotter. The crustal conductivity depends on the temperature and can be relatively low in hot neutron stars. Due to this, the field decay is rapid in young neutron stars with an age yrs. This type of behaviour has been well known since the paper by Urpin & Muslimov (1992). The fast decay has been studied in detail by a number of authors (see, e.g., Urpin & Konenkov 1997; Sengupta 1998; Mitra et al. 1999, etc.), and was rediscovered with no citation in recent calculations by Pons & Geppert (2007). However, even such efficient field decay during the initial stage can influence the thermal evolution only if the magnetic field is sufficiently strong and, therefore, our study primarily addresses high magnetic field pulsars.
2 The internal magnetic fields in pulsars
The unstable stage lasts only s in proto-neutron stars, but this is sufficient for dynamo action to generate a strong magnetic field because the turbulent motion is very fast. A turbulent dynamo can generate a large-scale magnetic field only if the star rotates rapidly and the rotation period is shorter than some “critical” value ( s in the simplest model). Most proto-neutron stars likely rotate faster and, as a result, a dynamo should operate in these objects (Bonanno et al. 2003, 2005). The dynamo generates both the toroidal field that is essentially internal and vanishes at the surface and the poloidal field that is non-vanishing outside the star. The poloidal field is responsible for pulsar activity. Typically, the generated toroidal field is comparable to the poloidal one if the proto-neutron star rotates rigidly, but it can be substantially stronger if rotation is differential. For example, the toroidal field is times stronger than the poloidal one if rotation at the center is three times faster than that at the surface equator. The saturation field generated by the dynamo can be estimated by making use of the simplest model of -quenching (Bonanno et al. 2006). This yields for the generated large-scale field
where is the equipartition small-scale field, where is the turbulent velocity. The equipartition field varies during the unstable stage, rising rapidly soon after collapse and then decreasing when the temperature and lepton gradients are smoothed. At the peak, G in the convective zone (Thompson & Duncan 1993) and G in the neutron-finger unstable zone (Urpin & Gil 2004). However, decreases and becomes smaller than the peak value as the protoneutron star cools down. The dynamo operates while the quasi-steady condition is fulfilled with being the cooling timescale and the turnover time of turbulence. The final strength of a generated small-scale magnetic field is approximately equal to at the moment when the quasi-steady condition breaks down and . If , we have where is the turbulent lengthscale. Then,
Estimate (2) yields G for the maximum possible lengthscale km and few seconds.
Substituting estimate (2) into expression (1), we obtain
The shortest possible period is likely ms and, hence, the strongest internal magnetic field generated by a dynamo can reach G. The field at the surface is usually weaker than the internal field generated by a dynamo (Bonanno et al. 2006). Note that generation is more efficient in the outer layers because the parameter that determines the efficiency of the dynamo is proportional to and the density gradient (see, e.g., Rüdiger & Kitchatinov 1993) but the latter is maximal in the outer layers.
If is longer than , then the large-scale dynamo does not operate in proto-neutron stars but the small-scale dynamo is still efficient. One can expect that such neutron stars have only small-scale fields with the strength G and have no dipole field. Likely, slow rotation with is rather difficult to achieve in proto-neutron stars, and the number of such exotic objects is small.
It is difficult to predict the final disposition of the magnetic field after turbulent motion stops. The magnetic configuration generated by the dynamo can be unstable, for example, if it contains a strong toroidal component. MHD instabilities can lead to a rapid evolution on the Alfvén time scale and form a configuration with comparable poloidal and toroidal fields (see, e.g., Braithwaite & Spruit 2006; Braithwaite & Nordlund 2006). Therefore, it is unlikely that the toroidal field is substantially stronger than the poloidal one in neutron stars. When convection is exhausted, both large- and small-scale fields evolve under the influence of ohmic dissipation and buoyancy. Likely, formation of the crust provides the most important influence on the evolution of magnetic fields at this stage. Soon after convection stops, the neutron star cools down to the internal temperature K at which neutrons and protons can form nuclei and clusters in matter with a density g/cm. When the temperature decreases progressively, nuclei can be formed at a lower density as well. Nuclear composition at high density is subject to many uncertainties and depends generally on the pre-history of the neutron star. For instance, the composition of the “ground state” matter (Negele & Vautherin 1973) differs noticeably from that of the “accreted” matter (Haensel & Zdunik 1990). The Coulomb interactions of nuclei leads to crystallization that occurs when the ion coupling parameter reaches the critical value (Slattery et al. 1980); is the mean inter-ion distance, and are the number density and charge number of ions, respectively; is the temperature, and is the Boltzmann constant. Then, the crystallization temperature is
where is the number of baryons per electron, and g/cm. For g/cm, the crystallization temperature is K. Therefore, the crust formation starts almost immediately after the end of the convective phase (or even before the end), and the magnetic field generated by the dynamo should be frozen into the crust.
3 Joule heating in the crust
Likely, the evolution of the magnetic field in the crust of hot neutron stars is mainly determined by the ohmic dissipation, and Joule heating has an important influence on the thermal evolution. The rate of Joule heating depends both on the geometry of the magnetic field and the conductive properties of the crust. In a strong magnetic field, the ohmic dissipation can be accompanied by Hall currents (Shalybkov & Urpin 1997, Hollerbach & Rüdiger 2002, 2004). These currents are non-dissipative since they do not contribute directly to the rate of Joule heating. However, the Hall currents couple different modes and alter the magnetic configuration by redistributing the energy among modes. In this way, the Hall currents can indirectly affecr the rate of dissipation. Note also that, because of the non-linear nature of the Hall currents, they can generate magnetic features at the stellar surface with a smaller lengthscale than the background magnetic field. This has been known since the paper by Naito & Kojima (1994) (see also Muslimov 1994, Shalybkov & Urpin 1997) who argued that some neutron stars may have strong disordered magnetic fields at their surface due to the Hall effect. The same conclusion recently was reached by Pons & Geppert (2007).
The influence of the Hall effect on the magnetic field is characterized by the Hall parameter, , where is the gyrofrequency of electrons and is their relaxation time, is the electron effective mass. The Hall effect is unimportant if , but it can influence the magnetic evolution if the field is sufficiently strong and . Indeed, numerical simulations (Shalybkov & Urpin 1997, Höllerbach & Rüdiger 2002, 2004) indicate that some acceleration of the decay can occur, particularly if the Hall parameter is very large, . This conclusion, however, turns out to be sensitive to the initial magnetic geometry. For a purely toroidal field, the Hall effect develops fine field structures, which cause the field to decay on the Hall time-scale rather than on a much longer ohmic time-scale. However, the presence of even a relatively weak poloidal field ( few per cent) changes the result drastically, and dissipation proceeds approximately on the ohmic timescale. Since the magnetic field in the neutron star should have a rather complex geometry with both the poloidal and toroidal components, we can expect that departures in the rate of Joule heating caused by the Hall effect have to be small compared to the case when the ohmic dissipation is acting alone. Note that some simplified models describe the influence of the Hall effect on the magnetic evolution in terms of the decay on the Hall timescale (see, e.g., Cumming et al. 2004). From a comparison with numerical modelling, it is seen that this naive picture is insufficient. The Hall timescale often characterizes the period of oscillations rather than the decay timescale of magnetic modes. Such an oscillatory behaviour of the decaying magnetic modes was first obtained by Urpin & Shalybkov (1997). Despite Pons & Geppert (2007) having confirmed the earlier finding by Shalybkov & Urpin (1997) and Höllerbach & Rüdiger (2002, 2004) that the Hall effect does not substantially accelerate dissipation of realistic magnetic configurations, Aguilera, Pons, and Miralles (2007) in their study of Joule heating in neutron stars assume confusingly that the Hall currents result in a fast decay of the magnetic field.
The field decay can also be influenced by the so-called Hall-drift induced instability if it occurs in neutron stars (Geppert & Rheinhardt 2002). These authors found that instability can occur which raises small-scale magnetic modes if the initial magnetic field is strong and its second spatial derivative is large enough. It is unclear, however, whether the effect of this instability on the dissipation rate is noticeable or not since a non-linear regime has not been considered. In particular, Hollerbach & Rüdiger (2002) express doubts that a linear instability starting from small amplitude perturbations can be compatible with the cascade caused by the non-linear Hall effect. Since even this cascade leads only to small departures in the dissipation rate for realistic magnetic configurations (Shalybkov & Urpin 1997, Höllerbach & Rüdiger 2002, 2004), the effect of a linear instability should be very weak, if it exists. As far as the non-linear regime of instability is concerned, Geppert et al. (2003) assume that, at saturation, the amplitude of unstable perturbations can reach a significant fraction of the background field and, hence, the latter should decay on the Hall timescale. Since this obviously contradicts the observed lifetime of pulsars ( yrs), the authors assume that the Hall drift induced instability can operate only during part of the neutron star life whereas decay before and after such episodes is determined by the ohmic dissipation. According to Rheinhardt & Geppert (2002), episodes occur when the age of a neutron star is yrs since the Hall parameter is not sufficiently large in younger stars. However, studies of pulsars based on methods of population synthesis (Bhattacharya et al. 1992, Hartman et al. 1997, Regimbau & de Freitas Pacheco 2001, Faucher-Giguere & Kaspi 2006) indicate that the magnetic field of radiopulsars decays little during their active lifetime. A significant magnetic field decay in radiopulsars likely can occur only in very young stars with age yrs since the number of these pulsars is small and they give a negligible contribution to any statistical analysis. Therefore, observations also do not support the idea of episodes of the Hall drift induced instability in neutron stars. Note that recent calculations of the non-linear field decay by Pons & Geppert (2007) confirm the conclusion by Hollerbach & Rüdiger (2002) that, even if the Hall-driven instability exists in neutron stars, it has no appreciable influence on the field decay.
4 Statement of the problem
To calculate the rate of Joule heating in young neutron stars, we consider a very simplified model. We assume that the magnetic field of neutron stars is generated by a turbulent dynamo at the beginning of their evolution. The dynamo -parameter is proportional to the density gradient and, hence, the dynamo is most efficient in the surface layers of proto-neutron stars (see Bonanno et al. 2005). Hence, one can expect that there exist electric currents in the outer crust just after the convective stage. The decay of currents is highly inhomogeneous since the electric resistivity depends on the density and varies by many orders of magnitude over the crust. The decay timescale is , where is the conductivity and is the lengthscale of the magnetic field, and currents deposited closer to the surface will decay faster because the conductivity is lower. Therefore, the thermal balance of young neutron stars with age yrs can be influenced only by dissipation of currents located in the surface layers.
The decay of the crustal magnetic field is governed by the induction equation without the convective term
where is the electric resistivity tensor and is the conductivity tensor. In a magnetized crust, components of the conductivity tensor are
where and are the components parallel and perpendicular to the magnetic field, is the so-called Hall component that determines the current perpendicular to both the magnetic and electric fields, is the coductivity at , and are the number density of electrons and their effective mass, is the gyrofrequency of electrons, and is the relaxation time. If the magnetic field is sufficiently strong and , then the conductivity components across the magnetic field and are suppressed, and only the conductivity along the magnetic field is essential. Components of the resistivity tensor are given by
where is the number density of electrons. In a strong magnetic field, the components parallel and perpendicular to the magnetic field are the same and are not suppressed by the magnetic field. The Hall component of resistivity can be higher than if that, generally, can be fulfilled in some layers of the neutron star.
We neglect the Hall term in our consideration and, strictly speaking, our results apply to neutron stars with not very strong magnetic fields. However, as was argued in previous studies (Urpin & Shalybkov 1997; Höllerbach & Rüdiger 2004; Pons & Geppert 2007), even in a very strong magnetic field that can magnetize plasma, the Hall effect insignificantly changes the rate of dissipation if the magnetic field contains a poloidal component. The difference in the rate of dissipation between the model that takes into account the Hall effect and the hypothetical model that has the same initial magnetic configuration but evolves in accordance with Eq. (5) without the Hall effect does not exceed 10-20%. This is much smaller than uncertainties in our knowlegde of the initial magnetic configuration or the chemical composition of the crust. Such accuracy is sufficient for our purposes, and we will mimic the field decay by Eq. (5).
We restrict our consideration to a dipolar field that can be described by the vector potential , where and are the radius and polar angle, respectively. The function obeys the equation
with the boundary conditions at the stellar surface and in the deep crustal layers. The -component of the electric current maintaining the dipolar magnetic field is
We have for the rate of Joule heating . For simplicity, nonsphericity is often neglected in cooling calculations. Therefore, we will use the polar-averaged expression for the rate of Joule heating. It is also convenient to normalize the function to its initial value at the surface, , which in turn can be related to the initial field strength at the magnetic equator by . Then, the polar-averaged rate of Joule heating is given by
In young neutron stars with age yrs, the conductivity of the outer crust and the outer part of the inner crust is determined by electron scattering on phonons. Scattering on impurities is important only in deep layers of the inner crust even if the impurity parameter is large (see, e.g., Jones 2004). We use the conductivity due to electron-phonon scattering calculated by Itoh et al. (1993). These conductivities depend on the temperature. Calculations presented here are based on the standard cooling scenario, which corresponds to a star with standard neutrino emissivities. We consider the field decay using the thermal history for the 1.4 neutron star constructed with the equation of state of Friedman & Pandharipande (1981) which is representative of intermediate equations of state. Our choice is compelled by the fact that models with the equation of state stiffer than that of Friedman & Pandharipande agree better with data on the magnetic evolution of pulsars (Urpin & Konenkov 1997).
Calculating the rate of Joule heating, we neglect its back influence on the thermal evolution of a neutron star. It is not the purpose of this paper to discuss in detail how the thermal and magnetic evolution are coupled. One can neglect this coupling if the rate of heating does not exceed the luminosity of a standard neutron star. Our approach allows us to obtain the lower limit on the field strength that can affect the thermal evolution due to Joule heating, and we compare this limit to observational data. Note, however, that even the temperature of magnetars which are believed to be heated by the decay of extremely strong fields G is only a factor higher than the temperature of a standard cooling neutron star. Therefore, our calculations can provide an order of magnitude estimate for the rate of Joule heating in the case of such strong magnetic fields. This simplified approach can be useful in understanding the main qualitative features of Joule heating in magnetars. A study of the coupled early magnetothermal evolution of very strongly magnetized stars such as magnetars is a more complicated problem, and it will be considered in a forthcoming paper.
If the field in the surface layers is very strong, such as where is the shear modulus of the crust, then the induction and momentum equations are coupled, and magnetic stresses can induce motion of the crustal material. Therefore, decay of the crustal magnetic field can change the Lorentz force and, generally, can lead to crustal motion. The shear modulus is where , and is the charge and number density of ions (Strohmayer et al. 1991). The condition is approximately equivalent to g/cm where G, and one should expect that Joule heating of the surface layers in high magnetic field pulsars is accompanied by motion in the crust. We will neglect, however, the contribution of this effect to heating.
5 Numerical results
In calculations, we assume that the magnetic field generated by a dynamo initially occupies the outer layer of the crust up to a density thus, initially, at . Since the field is confined to the crust, the density can be lower or equal to the density at the crust-core boundary, g/cm. It is difficult to determine the inner boundary of the generation region from the physical data since both turbulent dynamo coefficients and stability properties of proto-neutron stars are subject to many uncertainties. Therefore, we perform calculations for a few different values of . Note that the magnetic evolution is in good agreement with pulsar data if g/cm (Urpin & Konenkov 1997). This conclusion is in qualitative agreement with the dynamo models of neutron stars since the dynamo is efficient only in the surface layers where the density gradient is large. After the dynamo action stops in a proto-neutron star, the field diffuses into deeper layers and can be non-vanishing at . The initial distribution of the magnetic field at is also uncertain but, fortunately, the main qualitative results are not crucially sensitive to this distribution. We consider two models of the initial distribution shown in Fig. 1. These models differ by the characteristic depth of currents with model 2 (shown in the dashed line) corresponding to a smaller depth than model 1 (solid line).
In Fig. 2, we plot the distribution of the rate of Joule heating, , for different ages. The distribution turns out to be complicated with a deep minimum that originates because, for a dipole field, the current density changes sign at some depth. The depth of this minimum increases with time due to diffusion of the magnetic field into deep layers. The origin of this minimum is caused by the general diffusive properties of the crustal magnetic field and can be understood from the simplest qualitative consideration. Indeed, if the initial distribution of is like those shown in Fig.1, then the magnetic field will diffuse with time into deep layers with and, hence, the time derivative of will be positive somewhere at , at least. On the another hand, the value of and the field strength at the surface will obviously decrease with time because of ohmic dissipation and,hence, we have at . Since is a continuous function of the radius and has different signs at the surface and somewhere in deep layers, there always exists at least one point inside the neutron star crust where . Combining Eqs. (8) and (9), we find that at that point as well. Since , the rate of heating is also vanishing at the same depth. In Fig. 2, we do not show at this depth in detail because the region where is very narrow. The first maximum corresponds to a relatively low density g/cm, depending on the model. Initially, this maximum is located at a very low density, but it moves slowly inward with the time. After yrs, the maximum reaches a depth m corresponding to g/cm. At that time, the distribution of is already rather flat in the surface layers. The second maximum of is located substantially deeper, at densities g/cm, and it also moves inward with time. The position of the second maximum is less sensitive to the initial models because our models 1 and 2 differ mainly in the distribution of currents in the surface layers. Perhaps such a complicated distribution of can result in a complicated radial dependence of the temperature in strongly magnetized stars. The rate of heating can reach a very high value erg/cms or even higher if the initial magnetic field is stronger than G. The total rates of heating above and below the region where are of the same order of magnitude.
In Fig. 3, we plot the evolution of the density where the rate of Joule heating is maximal for models 1 and 2. This density corresponds to the first maximum of (see Fig. 2). The location of the layer where the maxumum energy is released is important for understanding the energy budget in neutron stars (see, e.g., Kaminker et al. 2006). During the initial yrs, the depth of this layer is very small and corresponds to g/cm. At this stage, depends on the initial distribution of currents. Later on, at yrs, this depth becomes almost independent of the initial distribution. Up to yrs, the maximum of Joule heating is located in the layers with a density lower than g/cm. Likely, heat released in the layers with such a low density will be transfered to the surface and emitted by photons rather than diffusing to the core and being emitted by neutrinos.
In Fig. 4, we show the evolution of the total rate of Joule heating integrated over the crust volume, . For comparison, we also plot in this figure the photon luminosity of a neutron star with standard cooling. If the initial magnetic field is strong and the corresponding heating rate is above the dotted line, our results can provide only an order of magnitude estimate because Joule heating will influence the neutron star thermal evolution. The rate of Joule heating is calculated for three values of , , and g/cm. For all these initial distributions of the magnetic field, the rate of Joule heating can reach rather high values erg/s during yrs if the initial field strength is G. This heating rate is higher than the luminosity of a standard neutron star without any additional heating mechanisms. At a given initial field strength, the heating rate is initially higher for smaller , but it decreases faster with the time. For example, if the magnetic field initially occupies the surface layer with a density g/cm, then the heating rate at yrs is approximately a factor of 10 higher than in the case of g/cm. However, the heating rate for g/cm decreases very rapidly and becomes smaller already after yrs. Generally, the rate of Joule heating can be high in young neutron stars. Even in pulsars with initial magnetic fields , Joule heating exceeds the photon luminosity during yrs if g/cm. Therefore, young pulsars with such magnetic fields should be hotter than it is predicted by the standard cooling scenario. High magnetic field pulsars such as PSR J1847-0130 ( G) or PSR J1718-3718 ( can be in such a “heated” state even longer ( yrs). However, after that time, their thermal evolution will follow the standard scenario. Our calculations show that even the rate of heating required for magnetars, erg/s, is reachable during the initial evolution if the initial magnetic field at the surface is G. Note that the rate of Joule heating depends not only on the field strength but also on the depth of the region where the magnetic field was generated. This dependence is rather sensitive and, generally, it is possible that the heating rate differs by more than an order of magnitude in pulsars of the same age and having approximately the same surface magnetic fields (for example, compare the solid and dash-and-dotted lines in Fig. 4). Such different heating rates can lead to a substantial difference in the surface temperature in high magnetic field pulsars.
We have considered dissipation of a magnetic field initially anchored to a neutron star crust. The magnetic field of neutron stars can be generated by a turbulent dynamo during a short hydrodynamically unstable phase at the beginning of their evolution. The mean-field dynamo is most effecient in the surface layers where the density gradient is large and, hence, the dynamo -parameter is maximal. Therefore, electric currents maintaining the magnetic configuration are likely located in the surface layers. Dissipation of electric currents is a highly inhomogeneous process because the density and, hence, conductivity varies by many orders of magnitude through the crust. The rate of dissipation decreases with increasing density and, hence, the field decay is slower in deep crustal layers. Dissipation of currents located in the surface layers proceeds on a relatively short time-scale and is accompanied by massive heat release. Joule heating is so efficient that it can even influence the thermal evolution of young neutron stars if the magnetic field is sufficiently strong.
The duration of the stage when Joule heating can affect the thermal evolution is determined by the strength of the magnetic field and the depth where this field is anchored. Both these quantities can vary over a wide range because they depend, for example, on poorly known details of the generation process and post-collapse hypercritical accretion that can essentially submerge the generated magnetic field (Chevalier 1989). At a given field strength, the rate of Joule heating is higher in a star where the field was initially anchored in the layer with a lower density. However, the time interval when this heating is important for the thermal evolution is shorter in such stars. On the contrary, if the field is anchored in a deeper layer, Joule heating is less effecient but it can contribute significantly in the thermal evolution over longer time.
Since the rate of Joule heating depends on two parameters it is generally possible that neutron stars with the same age and surface magnetic field can have substantially different heating rates and, hence, surface temperatures. This allows us to understand why the surface temperature of the high magnetic field pulsar PSR J1718-3718 is substantially lower than that of magnetars despite its magnetic field being approximately that of magnetars (). The magnetic field of high magnetic field pulsars was likely anchored initially in layers with a lower density, and the stage of efficient Joule heating when their luminosity was comparable to that of magnetars is completed.
Our calculations show that additional heating provided by dissipation of the crustal magnetic field can even be comparable to the luminosity of magnetars ( erg/s) if the magnetic field at the stellar surface is as high as G. Generally, such a strong magnetic field can be generated in rapidly rotating proto-neutron stars by the turbulent -dynamo (Bonanno et al. 2006). Note that our calculations provide only the lower limit on the rate of Joule heating since we neglected the back influence of this heating on the crustal temperature. Additional heating will increase the temperature and decrease the conductivity and, hence, it will result in a higher dissipation rate if one consistently takes into account the coupling between the thermal evolution and field decay. For strongly magnetized stars with a surface field G, the epoch when Joule heating is of the order of the magnetar luminosity can last as long as yrs if the magnetic field was initially anchored in the layers with g/cm. This time is comparable to the estimated life-time of magnetars. If the initial field is weaker. G, but is confined to the same layers, then the rate of Joule heating exceeds the standard luminosity of a cooling neutron star for a shorter time, yrs. During this time, the rate of heating is approximatelly one order of magnitude greater than the luminosity of a standard neutron star with the same age. Even in neutron stars born with a relatively weak magnetic field G, Joule heating can influence the early thermal elolution but for a very short time and only if the magnetic field was initially confined to low density layers.
From our results, we conclude that many young neutron stars can ehxibit departures from the standard cooling scenario if the magnetic field is of crustal origin and if it is sufficiently strong. How large these departures are and how long Joule heating can manifest is determined by the initial strength of the magnetic field and its location. At the moment, observations only provide information on the surface temperature of neutron stars with an age greater than kyr. For stars with such age, our model predicts that departures from standard cooling can be expected only if the magnetic field is sufficiently strong, G. Therefore, recently discovered high magnetic field pulsars such as PSR J1847-0130 ( G), PSR J1718-3718 ( G), PSR J1814-1744 ( G), PSR J1119-6127 ( G), and PSR B0154+61 ( G) all can have a higher surface temperature than is predicted by standard cooling models without additional heating.
In Fig. 5, we plot the available data on the surface temperature and magnetic fields of 22 young neutron stars. These data include 9 magnetars listed in Table 1 by Pons et al. (2007) which are likely young objects according to current theory. We also plot the data on and for 13 radiopulsars with a spin-down age shorter than 1 Myr. If the magnetic fields of these pulsars decay, their true age should be substantially less than the spin-down age and, likely, such pulsars are sufficiently young to be treated in our analysis. These 13 radiopulsars are listed in Table 1.
The surface temperature and magnetic field of young radiopulsars.
|RX J0822-4320||0.14-0.16||3.4||Zavlin et al.(1999)|
|Pavlov et al.(1999)|
|1E 1207.4-5209||0.12-0.16||0.35||Zavlin et al.(2004)|
|Gotthelf et al.(2007)|
|Vela||0.06-0.07||3.4||Page et al.(2004)|
|PSR B1706-44||0.07||3.0||Page et al.(2004)|
|PSR J0538+2817||0.075||0.8||Levandowski et al.|
|Geminga||0.043||1.6||De Luca et al.(2005)|
|PSR 1055-52||0.064||1.15||De Luca et al.(2005)|
|PSR B0656+14||0.077||4.7||De Luca et al.(2005)|
|PSR B2334+61||0.056||10||McGowan et al.|
|PSR J1718-3718||0.145||74||Kaspi at al.(2005)|
|PSR J1119-6127||0.206||41||Gonzalez et al.(2005)|
|CXOU J1819-1458||0.120||50||Reynolds et al.(2006)|
|PSR J1357-6429||0.085||8||Zavlin (2007)|
In accordance with our calculations, the thermal history of young pulsars with an age yrs can be influenced by Joule heating if the magnetic field at birth is stronger than G. Indeed, it seems that the surface temperature of high magnetic field pulsars with G shows some trend to be higher than that of low magnetic field pulsars, in qualitative agreement with the prediction of our model. This difference cannot be accounted for by the influence of the magnetic field on the thermal conductivity, because the geometry and strength of the magnetic field are unimportant for the surface averaged thermal structure of neutron stars if the field strength is moderate, G (Potekhin et al. 2005). For such , the magnetic field can affect the thermal evolution of neutron stars only via Joule heating, and the surface temperature should be proportional to approximately . The data in Fig. 5 obviously are not sufficient to prove this dependence but, at least, they do not contradict it. More detections of the surface temperature in high magnetic field pulsars are needed, and they could provide strong evidence of the crustal origin of the magnetic field in neutron star.
It is important to consider coupled magnetothermal evolution by solving the heat and induction equations because characteristic timescales of the thermal and crustal magnetic evolution are approximately comparable in young neutron stars with yrs. However, this problem, taking into account the magnetically-induced anisotropy of the thermal conductivity and electric resistivity tensors,is far from being solved and the study of particular problems of the magnetothermal evolution can help in understanding when Joule heating can affect neutron star cooling. From the result of the present study and conclusions obtained by Miralles et al. (1998), Joule heating can be important only in very young ( yrs) or in old ( Myr) neutron stars provided the magnetic field is sufficiently strong at birth. In stars with a moderate age, Joule heating seems to be inefficient.
This work has been supported by the Spanish Ministerio de Ciencia y Tecnologia grant AYA 2001-3490-C02. VU thanks Generalitat Valenciana and Universitat d’Alacant for a financial support and hospitality.
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text:
Gerard Butler may be holding back on some of the public outings with his girlfriend Morgan Brown after a crazy night of partying in London.
Seeing how ‘Phantom of the Opera’ star has revamped his New York apartment, possibly for Morgan Brown, the engagement rumors are beginning to make sense.
After ‘London Has Fallen’ filming, Gerard Butler may have his girlfriend on his mind more than ever.
Forbes recently did an article on Gerard Butler’s New York apartment and that got his fans thinking about whether he has engagement on his mind.
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‘Phantom of the Opera’ singer has been concentrating on ‘London Has Fallen’ filming as the rumors circulate around his girlfriend.
The rumor has it that Gerard Butler and Morgan Brown may be engaged after a rather short relationship history.
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She showed off the impressive ring as she was spotted taking in a solo stroll through Malibu, California.” When do you think Gerard Butler and his girlfriend will make their rumored engagement public? Let me know in the comments below!

domain: celebrity


text:
The show — a contemporary reimagining of Gaston Leroux's gothic novel "The Phantom of the Opera," set in the sexy and cutthroat world of the modern-day music business — will be executive produced by Marc Cherry and Sabrina Wind and their Cherry/Wind Productions.
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The team is also writing a stage musical based on the New Line Cinema feature "17 Again."

domain: artistic


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domain: design


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This question about the weight of a water glass explains the best way to deal with everyday stresses
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domain: news


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So the 17-year-old earned a little bit of downtime on Sunday night — and she got it with 25-year-old rapper Tyga!
Kylie and Tyga enjoyed a night out at Nobu in West Hollywood Sunday evening, heading to the restaurant in the rapper’s green Bentley.
In the shot, the reality star covered her face with her bag — no Kylie for you! — but was planted firmly next to Tyga in the passenger seat.
Kylie also posted a pic of her shoes — and the car — on Instagram, too (below):
├░┼╕ΓÇÿΓÇª├░┼╕ΓÇÿΓÇª├░┼╕ΓÇÿΓÇª├░┼╕ΓÇÿΓÇªA photo posted by King Kylie (@kyliejenner) on Jul 12, 2015 at 7:37pm PDT
It’s the first time the two have been spotted together since the scandal broke surrounding transgender model Mia Isabella and her alleged claims of a dalliance with Tyga.
Looks like Kylie is thus far stickin’ by her man!
[Image via AKM/GSI.]

domain: entertainment


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Journalists love to about new laws that will go into effect on January 1 because the story can be written in advance, before the holiday vacations kick in. New laws — unlike crimes, protests, or the making of new laws — sit still, just waiting to be implemented. And then there are old laws that get a new shine each year, because they were too complex to do all at once (see Care, Obama) or because they have been designed to be updated annually.
Oregon’s minimum wage increased this week to $9.10 per hour because it’s indexed to inflation. That amount was calculated and announced months ago, but it was barely considered newsworthy until the week when it is taking effect. When Oregon passed Ballot Measure 25 in 2002, it was considered a progressive milestone.
Now it’s an emblem of yesterday’s news.
Since then, and especially in the past year, minimum wage hikes have been the legislative lapel pins of liberal jurisdictions across the country. But another factor has also kicked in that Oregonians didn’t foresee in 2002.
While the national minimum wage remains stuck at $7.25, activists have learned to cherry pick mandatory wage hikes, which have not yet affected those who pick cherries. The movement often is bypassing states and targeting cities. San Francisco, San Jose, Washington, D.C. and Albuquerque, New Mexico are raising their minimum wages to double digits. Sea-Tec, which is barely even a township, is seeking to lead the nation with a $15 per hour minimum.
None of this is happening in Oregon, because it can’t.
Oregon’s 2002 ballot measure forbids it. As darling as that baby was to many of us, we didn’t notice the bathwater of local control. Oregon cities and counties lost their right to set their minimum wage higher than their neighbors when voters passed Measure 25.
Eugene has been aggressively promoting its own economic development for most of the past decade. The first order of business was to fill the holes and brighten the blight that had become downtown. The second priority was to increase the employment base, which is well underway. The focus next will turn to raising the average wage in Eugene, which has been lower than the state average for decades.
Raising the mandatory minimum wage above the state’s won’t be allowed. Attracting more CEOs to bring their corporate headquarters to Eugene won’t be easy. And building the strong middle for our local economy won’t be quick.
Here’s where you can throw up your hands, as if in surrender or in prayer, and let it go.
Or we can do something completely new. Instead of increasing the mandatory minimum wage, how about raising the voluntary minimum wage? Here’s how it could work.
The Eugene Area Chamber of Commerce or some other local non-profit organization devoted to economic development could offer all local employers a program that promotes their decision to treat their employees better than the required minimum. Any amount over the minimum would qualify a company to participate.
If a coffee kiosk’s lowest paid worker gets paid $12 per hour, will customers gladly pay an extra 20 cents for their espresso? I think we know the answer to that question. You might even begin to see coffee counters without tip jars. Perish the thought!
Customers will begin to ask how well lowest paid workers are compensated. Signs available only from the agency running the program will tell them, including a phone number to call if they know the posted number is untrue. The agency also would publish a directory of all participating businesses.
After that, the power shifts to the customers. They might frequent only participating businesses. They could change their shopping and buying habits to reward those places that pay their workers better. Shop owners will be competing for the best workers and the best customers in a way that furthers the economic goals of the city, without any governmental mandate necessary.
Eugene can’t prove its liberal bona fides by declaring its workers are more deserving than those doing the same work in neighboring towns, but it can do something better.
Don Kahle (email@example.com) writes a column each Friday for The Register-Guard and blogs.


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A memorial service will be held in Brant County on Oct. 8 for Ronald C. Davidson, who oversaw one of the biggest advances in fusion energy research.
Vincent Ball, Brantford Expositor
A graduate of the Master's journalism program at the University of Western Ontario and Glendon College, York University, Vincent Ball has been a reporter at The Expositor for the past 25 years. Now covering the police and business beat for The Expositor, Ball previously covered health, social services as well as education. In addition to writing stories, Ball produces videos for The Expositor's website and writes For What it's Worth, a weekly column. After work, Ball trains in the martial arts and works on other writing projects including one detailing the contributions of Brantford, Brant County and Six Nations to the First World War.
Vincent Ball Tweets
The community's ambulance service will need at least $2.5 million in new funding over the next 10 years, city councillors were told this week.
A new building for the Brant County SPCA moved one step closer to reality on Tuesday.
Earl Haig Family Fun Park is in need of upgrades and fire department officials are eager to get moving on a training facility for firefighters.
Niblet is getting a little old for walkathons.
Little Luke was surrounded by a lot of love on Sunday.
There is a new apple tree at W. Ross Macdonald School but it's not planted in the ground.
The 56th Field Regiment, Royal Canadian Artillery, renewed its bond with the city and celebrated a major milestone on Saturday.
City councillor are looking at ways to improve the safety of Brantford's extensive trail system.
The 150th anniversary of the 56th Field Artillery Regiment Royal Canadian Artillery will be recognized by Branford Mayor Chris Friel and members of city council on Saturday.
Officials at the Brantford food bank are asking residents to think about how they might address hunger in the community.
A self-described "modern renaissance man living the entrepreneurial dream" will be in Brantford next week.
Sharon Parker said that she is glad that a "radar feedback" sign has been installed near her home on a hydro pole on St. Paul Avenue, near Ada Avenue.
"We get calls almost on a daily basis from residents who have had to deal with pushy salespeople who try to force their way into homes," Const. Laura Collier said Monday.
That's one question many are asking following Wednesday's meeting about plans to build a bike park in Waterworks Park. The meeting, held by Ward 2 councillors John Sless and John Utley, attracted a capacity crowd at T.C. Costain Community Centre and lasted more than two hours.
Councillors this week applauded city staff for their efforts in the massive multi-million dollar cleanup after hearing a report from Tara Tran, the city's senior policy planner, and Nicole Wilmot, the manager of policy planning.
City councillors this week voted to ask staff to look into the possibility of program modelled on a city program that provides eligible property owners with a grant of up to $1,000 to replace lead water pipes. The resolution was brought to a council committee meeting by Ward 4 Coun. Richard Carpenter.
"We're really grateful to city council for their help and, of course, we really couldn't do this without such a great organizing committee," she said.
Christopher Starr, who died Friday in a motorcycle accident in Norfolk County, was a "real gentleman," says his widow.
For the second time this year, local Liberals have elected a new riding association executive committee at an annual general meeting.


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Zsofia Wagner @zsofiawagner
This is a yearly event, in the Botanical garden, 40 days long every evening a yoga session takes place. (in case of bad weather indoor in the hall). please feel free to join every evening or a certain evening. the session starts @18:30. please bring with you -yoga mat -comfy clothes -blanket for the long deep relaxation -meditation cushion -water it is a charity event, you can donate as much as you wish. the language of the sessions is german, still it is easy to follow, and a good training;-) we are going to meet in front of the garden, 15 minutes before start.
Botanischer Obstgarten Heilbronn
Yoga in the Botanical Garden
Sunday, June 30, 2019
6:15 PM - 7:15 PM


Savage Arms Axis 308win Bl-syn 22″ Pkg
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Xiaomi Mi 10T Pro 5G smartphone is going to be launched on 3rd Nov 2020. The phone Flash sale is started on Flipkart on 3rd nov 2020. The mobile phone has 6.67-inch touchscreen display with a resolution of 1080×2400 pixels. It has dimension of Height: 165.1 mm x Width: 76.4 mm x Thickness: 9.3 mm and weight 218g.
Mi 10T Pro phone come up with 2.84 GHz octa-core Qualcomm Snapdragon 856 processor. It has 8 GB of RAM. The Mi 10T Pro 5G have Android 10 (Q) and is has massive battery backup of 5000mAh non-removable battery. The Mi 10T Pro 5G supports proprietary fast charging.
The Mi 10T Pro phone has rear camera of 108-megapixel primary camera with an f/1.69 aperture (up to 30x Digital Zoom); 13-megapixel camera with an f/2.4 Wide Angle, Ultra-Wide Angle Camera; 5-megapixel camera with an f/2.4, Macro Camera. The rear camera setup has autofocus. It has Front camera of 20-megapixel f/2.2 Wide Angle Primary camera for selfies.
The Xiaomi Mi 10T Pro phone comes with MIUI 12 with Android 10(Q) and 128 GB of inbuilt storage. The Mi 10T Pro 5G has a dual-SIM mobile phone that accepts Nano-SIM and Nano-SIM cards.
The phone will be launched in Cosmic Black, Aurora Blue and Lunar Silver colors.
Connectivity options in the Mi 10T Pro 5G mobile phone include Wi-Fi 802.11, a/b/g/n/n 5GHz, MIMO, GPS with A-GPS, Glonass, Bluetooth v5.1, USB Type-C, FM radio, 3G, and 4G with active 4G on both SIM cards and it also supports 5G connectivity.
Sensors in the smartphone include accelerometer, ambient light sensor, compass/ magnetometer, gyroscope, proximity sensor, side fingerprint sensor and it also supports face unlock.
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Mi 10T Pro 5G Price in India
The Mi 10T Pro mobile phone price in India is starting from Rs 39,999. It is going to be launched in the country on Flipkart on 3rd nov,2020.
Specifications of Xiaomi Mi 10T Pro 5G
- OS: Android v10 (Q)
- Ram: 8 GB
- Storage: 128 GB + Not Expandable
- Battery: 5000 mAh
- Camera(Rear + Front): 108 MP + 13 MP + 5 MP Triple Camera; 20 MP Front Camera
- Processor: Octa core (2.84 GHz, Single core, Kryo 585 + 2.42 GHz, Tri core, Kryo 585 + 1.8 GHz, Quad core, Kryo 585)
- Display: 6.67 inches (16.94 cm) IPS LCD
- Chipset: Qualcomm Snapdragon 865
- GPU: Adreno 650
- Resolution: 1080 x 2400 pixels
- Weight: 218 g
- Charging: Fast, 33W: 100 % in 59 minutes
- Fingerprint: Side
- Bluetooth: v5.1
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On Hagel's first Afghan visit, Karzai alleges US, Taliban are colluding
March 10, 2013
KABUL – One day after a deadly suicide bombing rocked central Kabul, a press conference scheduled for Sunday with Afghan President Hamid Karzai and visiting U.S. Defense Secretary Chuck Hagel was canceled because of a security concern, U.S. officials said.
Hagel’s first trip to Afghanistan as defense secretary was marred not only by security issues, but by a series of harsh statements from the mercurial Karzai, who implied Sunday the United States and the Taliban share common goals.
Hagel was also forced to reschedule a meeting Sunday with the Afghan defense minister at the Defense Ministry building, where a suicide bomber on Saturday had killed 10 people. That meeting and another with the Afghan interior minister were held at another location, officials said.
A contradictory statement released by the Afghan presidential palace on Sunday, however, claimed that the cancellation was due to “scheduling pressure.”
A Sunday night meeting and dinner between Hagel and Karzai went on ahead as planned. Hagel said he directly addressed inflammatory statements about the U.S.-Afghan relationship Karzai had made earlier in the day, when Karzai seemed to accuse the United States and the Taliban of colluding to foment violence and fear in Afghanistan.
“I spoke clearly and directly,” about the "untrue" statements, Hagel said. But he declined to report Karzai’s response.
Hagel said the meeting overall was a productive discussion of the major issues confronting Afghanistan, and that he had urged Karzai to telephone him directly for any needed assistance.
Karzai earlier in the day had been far less conciliatory.
According to a translation provided by the NATO-led International Security Assistance Force personnel and described as hastily prepared, Karzai claimed the suicide blast at the Defense Ministry on Saturday, and a second bombing that killed eight people in Khost province, benefit the United States.
“Yesterday’s attack was not against the U.S., it was in their favor,” he said. “It adds to the fear of 2014, and it strengthens the presence of American and foreign forces in Afghanistan.”
The Taliban are working for the benefit of the United States, Karzai said.
"The explosions in Kabul and Khost yesterday (Saturday) showed that they are at the service of America and at the service of this phrase: 2014,” Karzai said during a nationally televised speech about the state of Afghan women, according to The Associated Press. “They are trying to frighten us into thinking that if the foreigners are not in Afghanistan, we would be facing these sorts of incidents.”
A senior U.S. official speaking on the condition of anonymity said the claims are baseless.
“This is simply incorrect,” the official said. “The United States and the government of Afghanistan share a common view of the Taliban, and that is that they’re the enemy.”
The United States is committed to working with Karzai, but the president should temper his public statements, the official said.
“We have indicated to him in private that public criticism is unhelpful to the partnership, especially when there is no basis in fact for some of the claims he makes,” the official said.
Karzai wasn’t finished, however, and later demanded that coalition troops stop abusing Afghan university students and stay off campuses.
That charge prompted a response from the U.S. commander in Afghanistan, Gen. Joseph Dunford.
“There are no members of the coalition that are harassing university students,” he told journalists Sunday.
Karzai has a history of drawing attention with such statements, in one case threatening to join the Taliban himself. In recent weeks he has disagreed with the United States over issues including coalition airstrikes in support of Afghan forces and custody of Afghan prisoners.
Dunford said that despite such flare-ups on the public stage, he privately has a good working relationship with Karzai and other top Afghan leaders.
“I don’t know why President Karzai might be doing this, but I understand difficult negotiations, I understand the issues that have been raised,” Dunford said. “I guess his perspective is that maybe it’s productive to air these differences in public.”
Hagel is in Kabul to discuss the transition of security responsibility from the United States to Afghan forces as the NATO combat mission here moves toward an end in December 2014.
Early Sunday, he traveled to the Kabul Military Training Center, the largest training installation for Afghan army troops in the country. There, the former Army sergeant who served in Vietnam saw some of the training Afghan non-commissioned officers undergo.
The United States and Afghanistan currently are negotiating the size and scope of a post-2014 force that President Barack Obama has said would remain in the country solely to train Afghan troops and conduct counterterrorist operations against al-Qaida and its affiliates, but not to carry on the current war.
Karzai charged U.S. and Taliban representatives are in “daily negotiations” outside Afghanistan, and said the United States has said it no longer considers the Taliban its enemy, according to The AP.
Karzai has presented other difficulties in recent weeks as well, clamping down on U.S. support activities for Afghan troops.
After the deaths of civilians in NATO coalition airstrikes in February, he forbade Afghan troops from calling in airstrikes while fighting the Taliban.
And in late February, after villagers’ reports of killings and kidnappings by U.S. troops – hotly disputed by coalition officials – Karzai demanded that U.S. special operations troops leave Wardak province near Kabul by Monday. The demand strikes at the heart of the U.S. strategy of training Afghan troops to take over the fight against the Taliban once the NATO combat mission here ends.
Dunford said that for now, special operators remain in Wardak, but said he had committed to develop a specific transition plan for the province so Afghan troops can take over for the Americans as soon as possible.
firstname.lastname@example.org Twitter: @ChrisCarroll_


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A Roma fan has been jailed after being a part of the pre-match violence outside Anfield in April.
The Italian club fans were involved in a number of incidents around the Liverpool FC ground before their Champions League semi final.
AS Roma fan Daniele Sciusco was arrested and charged following the clash.
He admitted violent disorder in court.
He has been sentenced to two and a half years in prison for his role in the violence.
On the same night but in a separate incident, dad-of-three Sean Cox suffered serious head injuries.
He was kept at Walton Neurological Centre until May, where he was moved to Beaumont Hospital.
Cox, from Dunboyne, County Meath, sustained a severe bleed on brain and underwent a major operation before doctors put him in an induced coma.
Judge Mark Brown said:
"During the past few years, the British police have done a great deal to try to eradicate this kind of mindless public disorder.
"They're doing that so that people can attend football matches without the fear or violence and intimidation.
"Young people are often present and it is for many a family occasion.
"You had traveled from Italy for the game and were a visitor to this country.
"The Liverpool people had welcomed the Italian supporters with their usual Scouse generosity.
"Your actions were a slap in the face to that hospitality.
"You have tarnished the reputation of Italian football supporters and Italian football.
"Bottles were thrown and during the early part of the incident Sean Cox was struck.
"That caused him to fall over and strike his head on the floor.
"His brother went to his assistance and was assaulted as well.
"The footage shows that you were close by when it happened, though I am keen to stress you were not directly responsible for that assault.
"Nonetheless it did occur during the violent disorder in which you were a willing participant and it is relevant to the level or harm caused by it."

domain: law


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Hey y’all! After a few months (more off than on) of stitching images together, I’ve mapped out every room in Quest for the Toa/Tales of the Tohunga! Give them a look and let me know what you think!
That’s pretty cool. Reminds me of the art style for Golden Sun a bit, though that’s probably because it’s the only other game I’ve really played from the era. Anyways, good work.


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Celebrate National Cheesecake Day at Cheesecake Factory!
July 29th and 30th you can get cheesecake 50% off. No coupon is needed.
This offer is for dine in only but we have often eaten lunch IN the restaurant and then gotten the cheesecake to go (one per person).
Plus, beginning July 29th they are debuting a new cheesecake- Chocolate Hazelnut Crunch Cheesecake- topped with hazelnut crunch and Nutella® on a blonde brownie crust.


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New details emerge regarding Doppler blind spots in Brunswick County
No indication that project expedited after deadly February tornado
BRUNSWICK COUNTY, N.C. (WECT) - It’s been nearly six years since the federal government confirmed there were serious issues with their KLTX Doppler radar in Shallotte. The beams the radar uses to read the weather there are partially blocked by pine trees on surrounding properties. The trees were not an issue in 1994 when the radar was installed, but they’ve grown so tall since then that they are now causing significant interference.
Specifically, the tree line has created a blind spot for the radar to the south and southwest, making it considerably harder for meteorologists to accurately forecast severe weather in time to warn residents in Ocean Isle Beach, Sunset Beach, and the Grand Strand. Many storms that impact our area approach from that direction.
Meteorologists have been complaining about the issue for years, but the problem came to the forefront again after a tornado hit Brunswick County in February, killing three people. There was no Tornado Watch issued in advance of the storm, and the Tornado Warning was issued as the storm was touching down, leaving those in the early path of the storm with essentially no warning to take cover. The fast-moving storm came directly up the path where the radar is partially blocked.
Despite the renewed concerns, there appears to be little to no progress in the plans to permanently fix the problem. Federal officials say buying the land surrounding the radar so they could remove the trees was not feasible, so moving the radar to a new location is the preferred path forward.
However, Maureen O’Leary, Deputy Director of Public Affairs for the National Weather Service, said they have yet to begin the process to find a more suitable location for the radar. She released the following statement in response to questions from WECT:
“As you know a forest has grown in the privately-owned land around the National Weather Service Doppler radar in Wilmington, NC. The trees block the lowest level radar scan, particularly to the southwest and south. We are exploring options to address the beam blockage problem, including a long-term solution to relocate the radar, but a location has not been identified.
Typically, the process involves identifying three possible locations and conducting an environmental impact assessment at each location to determine the most suitable site. That work has not started yet. Relocating the radar will take roughly three years and it is costly, estimated at $5.5 million. The timeline to begin the work depends on budget, but could begin about one year after funds become available.
We have implemented changes to improve coverage. On 11/17/20 we lowered the radar beam to 0.3 degrees at the Charleston, SC (KCLX) radar, which provides some additional coverage. We also implemented a new rain rate capability in November 2020, enabling improved precipitation estimates in areas with partial beam blockage.”
A public records request to Brunswick County for any additional information on heightened efforts to move the Doppler indicated the county had requested additional information from federal officials about what kind of site they would be looking for if the radar was moved. Just days after the storm, in an email to Brunswick County Emergency Services Director Ed Conrow and Deputy Director Scott Garner, NOAA Meteorologist Mark Willis wrote, “Any site would need a 1200ft radius with no objects 30m or higher and would need to consider the neighboring topography, partner considerations, and any new gaps that could be introduced.”
Copyright 2021 WECT. All rights reserved.


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There are many ways to mark a 10 year milestone and in Sun Peaks the period 2000 to 2009 is remembered for its great promise, rapid growth, devastating fires and sense of community that took root in the village.
Many remember the Delta fire of 2001 as a pivotal moment in the resort’s history. The community came together to help fight the blaze and begin the reconstruction process that helped relaunch the landmark hotel. Arguably lesser known, but no less devastating, was the McGillivray fire of 2003.
Started by lightening, the McGillivray fire was one of several that ravaged the Thompson Okanagan that year. For Dan Yano, a professional forest firefighter at the time, and his bride Suzanne Evans, the McGillivray fire lives in their memories as the one that caused the evacuation of their
“The day of our wedding, my groomsmen and I went golfing and we were getting showered with ash,” Yano recalls. “We had an inkling that (the fire) was getting closer to us.”
As the two were saying their “I do’s” the fire had advanced to within five kilometres of the resort and the 180 guests celebrating with them. The reception was well underway when they got the order to evacuate.
“I think it was amazing,” says Evans. “Everybody rallied around and I remember people’s faces looking devastated that it happened, but, at the same time, we were saying ‘we’ll always remember it!’”
It does take time but, after a wildfire comes new growth. As the decade marched on, and the fires became memories, Sun Peaks continued its rapid growth as more and more people chose to make the resort their year-round residence. Local business owners Dan and Terra Stebner felt that starting a business and raising a family in Sun Peaks was akin to pioneering.
“I’ve said this before, but where else in Canada, today, can you go and be a part of a community that was starting from scratch,” wonders Dan Stebner. “It was very appealing to us to grow our company and our family in Sun Peaks.”
And grow their family they did. November 12, 2006 started out blustery and just got worse as an early winter storm dumped 30 centimetres of snow on Sun Peaks in less than a day. Although they had hoped to home birth their expected child, by the time Terra went into labour, the weather provided them no choice of travelling down the mountain to deliver in the hospital. Instead, the Stebner’s second child, Theta, was born at home with the help of the Sun Peaks Fire Rescue Captain Riccardo Passeri, and Kamloops residents Dr. Walter Rees, and his wife Kathy, a retired emergency room nurse, who happened to be cross-country skiing at the resort that weekend.
“It was a pretty crazy two hours,” remembers Stebner, a volunteer member of the Sun Peaks Fire Department who had a fire truck complete with sirens and lights sent to retrieve the doctor from his home at Trapper’s Landing.
“The fire truck ran up and got him and in our bedroom on Burfield Drive there’s me, Terra and six members from the Fire Department waiting for him,” he recalls. The Stebners welcomed their daughter to the world within a half hour of the doctor’s arrival.
The Stebners had always felt like Sun Peaks was “their” community, but it took the arrival of their daughter to open new doors.
“For us, it was really neat, because we had a bunch of people that we didn’t know well, but when the baby was born at Sun Peaks, we made a lot of great friends,” grins Stebner.
In order for community to flourish it takes time, commitment and a group of people dedicated to supporting each other. The events of the last decade have proven that to be true in Sun Peaks.
Help us bring you more local news
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