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Researchers develop new architecture for lithium-ion battery anodes that far outperform the current standard
Researchers at the University of California, Riverside Bourns College of Engineering have developed a three-dimensional, silicon-decorated, cone-shaped carbon-nanotube cluster architecture for lithium ion battery anodes that could enable charging of portable electronics in 10 minutes, instead of hours.
Mihri and Cengiz Ozkan, both professors in the Bourns College of Engineering.
Lithium ion batteries are the rechargeable battery of choice for portable electronic devices and electric vehicles. But, they present problems. Batteries in electric vehicles are responsible for a significant portion of the vehicle mass. And the size of batteries in portable electronics limits the trend of down-sizing.
Silicon is a type of anode material that is receiving a lot of attention because its total charge capacity is 10 times higher than commercial graphite based lithium ion battery anodes. Consider a packaged battery full-cell. Replacing the commonly used graphite anode with silicon anodes will potentially result in a 63 percent increase of total cell capacity and a battery that is 40 percent lighter and smaller.
In a paper, Silicon Decorated Cone Shaped Carbon Nanotube Clusters for Lithium Ion Battery Anode,recently published in the journal SMALL, UC Riverside researchers developed a novel structure of three-dimensional silicon decorated cone-shaped carbon nanotube clusters architecture via chemical vapor deposition and inductively coupled plasma treatment.
Lithium ion batteries based on this novel architecture demonstrate a high reversible capacity and excellent cycling stability. The architecture demonstrates excellent electrochemical stability and irreversibility even at high charge and discharge rates, nearly 16 times faster than conventionally used graphite based anodes.
The researchers believe the ultrafast rate of charge and discharge can be attributed to two reasons, said Wei Wang, lead author of the paper.
One, the seamless connection between graphene covered copper foil and carbon nanotubes enhances the active material-current collector contact integrity which facilitates charge and thermal transfer in the electrode system.
Two, the cone-shaped architecture offers small interpenetrating channels for faster electrolyte access into the electrode which may enhance the rate performance.
Wang is a graduate student advised by Cengiz S. Ozkan, a mechanical engineering professor at UC Riverside’s Bourns College of Engineering; and Mihrimah Ozkan, an electrical engineering professor. Both of them are co-authors of the paper.
Other co-authors are Isaac Ruiz, Kazi Ahmed, Hamed Bay, Aaron George, who are all graduate students, and Johnny Wang, an undergraduate student.
Thermo-Optical Measuring method (TOM) could save several million tons of CO2 in coal-fired plants
25.05.2016 | Fraunhofer-Institut für Silicatforschung ISC
Atomic precision: technologies for the next-but-one generation of microchips
24.05.2016 | Fraunhofer-Institut für Lasertechnik ILT
A biological and energy-efficient process, developed and patented by the University of Innsbruck, converts nitrogen compounds in wastewater treatment facilities into harmless atmospheric nitrogen gas. This innovative technology is now being refined and marketed jointly with the United States’ DC Water and Sewer Authority (DC Water). The largest DEMON®-system in a wastewater treatment plant is currently being built in Washington, DC.
The DEMON®-system was developed and patented by the University of Innsbruck 11 years ago. Today this successful technology has been implemented in about 70...
Permanent magnets are very important for technologies of the future like electromobility and renewable energy, and rare earth elements (REE) are necessary for their manufacture. The Fraunhofer Institute for Mechanics of Materials IWM in Freiburg, Germany, has now succeeded in identifying promising approaches and materials for new permanent magnets through use of an in-house simulation process based on high-throughput screening (HTS). The team was able to improve magnetic properties this way and at the same time replaced REE with elements that are less expensive and readily available. The results were published in the online technical journal “Scientific Reports”.
The starting point for IWM researchers Wolfgang Körner, Georg Krugel, and Christian Elsässer was a neodymium-iron-nitrogen compound based on a type of...
In the Beyond EUV project, the Fraunhofer Institutes for Laser Technology ILT in Aachen and for Applied Optics and Precision Engineering IOF in Jena are developing key technologies for the manufacture of a new generation of microchips using EUV radiation at a wavelength of 6.7 nm. The resulting structures are barely thicker than single atoms, and they make it possible to produce extremely integrated circuits for such items as wearables or mind-controlled prosthetic limbs.
In 1965 Gordon Moore formulated the law that came to be named after him, which states that the complexity of integrated circuits doubles every one to two...
Characterization of high-quality material reveals important details relevant to next generation nanoelectronic devices
Quantum mechanics is the field of physics governing the behavior of things on atomic scales, where things work very differently from our everyday world.
When current comes in discrete packages: Viennese scientists unravel the quantum properties of the carbon material graphene
In 2010 the Nobel Prize in physics was awarded for the discovery of the exceptional material graphene, which consists of a single layer of carbon atoms...
24.05.2016 | Event News
20.05.2016 | Event News
19.05.2016 | Event News
27.05.2016 | Awards Funding
27.05.2016 | Life Sciences
27.05.2016 | Life Sciences


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Download PinballDroid apk 1.8 free for Android smartphone
Apk file size: 1.7 MB
Get a High score playing this new pinball game only for Android.
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DELCASDA PRODUCTIONS part of our Arcade and have average installs from 50 to 100. Last Update April 1, 2013. Google play rating is 50.0. Current verison is 1.8. Actual size 1.7 MB.

domain: game


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Aston Villa journalist Mat Kendrick has been discussing winger Trezeguet after the Egyptian scored a brace in Villa's 2-0 win over Crystal Palace at the weekend. This comes after Kendrick recentl
by: Scott Morris — 101 Great Goals 23h
Everton FC vs Aston Villa live streaming & betting tips: Premier League live streaming & live stream video, betting tips, prediction & odds. How to watch, head to head (H2H) information and best bets.
by: N/A — BBC 11 Jul
Liverpool came up against an outstanding Nick Pope - but how does the keeper compare to other English stoppers?
by: email@example.com (Chris Beesley) — Liverpool Echo 11 Jul
Liverpool have had some memorable matches against Burnley in recent seasons
by: Ian Herbert — Daily Mail 10 Jul
EXCLUSIVE BY IAN HERBERT: A Facebook memory popped up on Nick Pope's phone the other day to remind the Burnley goalkeeper, just how far he has travelled in 10 extraordinary years.
by: Duncan Mitchell — 90min 10 Jul
It could very well be Aston Villa's last shot at survival this Saturday with a crucial home tie against mid table Crystal Palace, where anything but three point
by: firstname.lastname@example.org (Tom Seymour) — Sheffield United News 10 Jul
Sheffield United forward David McGoldrick was instrumental in Premier League players taking a knee and explains why Black Lives Matter is so important.
by: N/A — EPL: Crystal Palace Football Club 10 Jul
The stats do not bode well for Aston Villa ahead of their clash with Crystal Palace on Sunday (12th July).
by: Freddie Keighley — Mirror Online 9 Jul
Manchester United will look to continue their assault on the top four when they take on Aston Villa at Villa Park on Thursday night. Kick-off 8.15pm (UK)
by: Vincent , Paul Clarke) — Birmingham Live 9 Jul
Is Aston Villa vs Manchester United on TV? What time does the game kick off?
by: Metro Sport Reporter — Metro News 9 Jul
Can United make it 17 unbeaten?
by: Charlie Horner, Manchester United Content Manager — Last Word On Sports: Last Word On Football 9 Jul
Manchester United will be eager to continue their chase for the top four as they travel to face the relegation-threatened Aston Villa.
by: MOMS — MOMS Aston Villa Blog 9 Jul
You only have to compare Aston Villa's three fit strikers with Manchester United's impressive trio's goals tally to get an uneasy feeling about the fixture.
News in the Past 30 days
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domain: news


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London, UK, June. 2, 2020 – Interxion, a leading European provider of carrier and cloud neutral colocation data centre services and a Digital Realty (NYSE: DLR) company, today announced a new partnership with RStor, the leading provider of cloud services across any multicloud environment. The partnership enables Interxion customers access to RStor’s performance-based cloud management services, including easy-to-use tools to manage backup storage, disaster recovery, and archival of data. This new service offering is directly accessible via Interxion’s London campus, where RStor has positioned its first Point of Presence. The service is also available to all customers at all Interxion’s other sites via Cloud Connect.
Using RStor, Interxion Cloud Connect customers can now deploy scalable, resilient network infrastructure and benefit from enterprise performance management across multiple public Cloud Services Providers (CSPs) without vendor lock-in or product complexity. Designed for cloud native workflows, RStor connects customer environments with cloud service providers through its innovative fabric technology. It delivers object-based, secure cloud storage through a single interface that allows customers to manage and scale data, and unlike traditional CSPs, RStor provides flexible access to multiple cloud storage systems to help users increase innovation and achieve unprecedented cost savings in virtual environments. Enterprises looking to invest in emerging technology services such as AI and Big Data analytics, can produce High Performance Computing (HPC) environments at Interxion London whilst also taking advantage of RStor’s agile, cloud agnostic management portfolio.
Andrew Fray, UK Managing Director at Interxion, added:
‘We are delighted that Rstor has chosen London as their first location with Interxion in Europe and that they are able to launch amid turbulent times. Rstor’s product line up complements our other cloud products and we anticipate that companies in several key sectors of London’s communities of interest, such as law firms, digital media companies and healthcare want and need object storage close at hand’.
‘Companies looking to invest in emerging technology services such as AI and Big Data Analytics, can roll out High Performance Computing (HPC) environments at Interxion London, while also utilising RStor’s agile, cloud agnostic management portfolio’.
Conor Malone, Chief Information Officer at RStor has commented: “We are excited about working with Interxion to bring the RStorage service to customers across Europe. Interxion provides RStor with the high carrier density and partner ecosystem that enables RStor's storage to be a single cross connect away from as many of our customers as possible.”
Interxion, a Digital Realty company, is a leading provider of carrier- and cloud-neutral colocation data centre services in Europe, serving a wide range of customers through more than 50 data centres in 11 European countries. Interxion’s uniformly designed, energy-efficient data centres offer customers extensive security and uptime for their mission-critical applications. With over 700 connectivity providers, 21 European Internet exchanges, and most leading cloud and digital media platforms across its footprint, Interxion has created connectivity, cloud, content and finance hubs that foster growing customer communities of interest. For more information, please visit www.interxion.com/uk.
RStor, is innovating on behalf of customers to deliver efficient, secure and easy to use cloud services. RStor was built by a founding team steeped in innovation in enterprise infrastructure, RStor equips customers with a single, integrated platform that eliminates variable costs, vendor lock-in, and regionality, while offering the flexibility of using multiple cloud service providers without additional fees. For more information, visit Rstor.io.


This cute Tiger Costume includes one piece bodysuit, hood with ears & plush ruff and booties. Inner leg snap closures on this Tiger Tot baby costume makes diaper changing a breeze. This cute tiger baby costume is cuddly soft and has feet with skid resistant bottoms. Care Instructions: Machine was cold, gentle cycle. Hang dry. Do not iron.
- Hood with plush details and bodysuit with snaps for easy diaper change and skid resistant feet.
- Toddler 12-18 months. Includes a soft jumpsuit with slip-resistant feet and a cute little tiger hood.
- Material content: polyester (exclusive of decorations)
- Care instructions: machine wash.


|Letterman's 2010 book, Late Show Fun Facts- |
from At The Matinee's vast media archive!
Through his two shows, Late Night With David Letterman on NBC from 1982-1993, and the Late Show on CBS, we have seen many personalities, dignitaries, and iconic guests on the series- such as Bill Murray, Regis Philbin, Oprah Winfrey, Steve Martin, Meredith Viera, celebrated newsman Tom Brokaw, Martin Scorsese, Billy Crystal, Jerry Seinfeld, "Jungle" Jack Hanna, Keith Olbermann, Stephen Colbert, Patrick Stewart, Rachel Maddow, Jay Thomas and his famous "Lone Ranger" story (during the holiday season), Presidents Jimmy Carter, Bill Clinton, and Barack Obama.
His shows have had many iconic segments- such as Stupid Human Tricks, Dave's Record Collection, Small Town News, Know Your Current Events, Stupid Pet Tricks, and most famously- the Top Ten list.
Let's not forget Letterman's Late Night/Late Show crew- bandleader Paul Shaffer, Biff Henderson, Tony Mendez, Pat Farmer, Hello Deli owner Rupert Jee, and Alan Kalter- who took over announcement duties when veteran announcer Bill Wendell (1924-1999) retired in 1995.
Letterman's announcement can be seen on the official CBS Late Show YouTube channel. CBS News also reported on his announcement hours before Thursday night's broadcast of the program.
Late Night television will never be the same again once Letterman steps down as host in 2015.
*Denotes this writer's preferred comedic picks in addition to Letterman and Kimmel, along with Craig Ferguson, Jon Stewart, Stephen Colbert, and Conan O'Brien. Of course, there will always be the "original king of late night", Johnny Carson (1925-2005).


I know someone on BigSoccer.com posted that this two-month road trip was almost like the offseason. I have to agree. But at least we get to see some action again after two weeks off.
First, just watched KC news conference from Thursday. Coach Onalfo said that Sasha Victorine will be back in the starting lineup. So, if Sasha starts then either Pore, Jewsbury, Marinelli or Zavagnin will not …
Micheal Harrington has a more pronounced mohawk. This looks to be what Bob Luder based his Harrington story off of. MH talks about his attacking abilities and playing midfield last year. And glad he was able to play left back at the end of last season.
Also Micheal is very bold. Says KC is better than the teams we are playing and that the goal on the road should be 3 points and not just 1. He was pretty confident.
Weahter update. Looks like 14 to 15 mph winds. Game will start out cloudy and will probably go to thunderstorms.
Also don’t forget, the Brass are playing in Colorado in a match that doubles as a USOC qualifier.


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LAND USE COMMITTEE
Norman Myers, Chairperson
Mission: To improve land use regulations and practices in the five counties of the Friends program area (Loudoun, Clarke, Fauquier and Rappahannock in Virginia and Jefferson in West Virginia) so that they continue to preserve and enhance the Blue Ridge Mountains as a valued resource and treasured space for future generations. As chair of the Land Use Committee, Norman Myers represents FBRM on the Loudoun County Preservation and Conservation Coalition. He participated on the SWAT Team (an advocacy group for the Loudoun County 2019 Comprehensive Plan). He continues to participate in the Zoning Ordinance Rewrite (ZOR) Committee (advocation for Improving Cluster Design in the Rural Planning Area), and the Committee for addressing Loudoun County’s Unmet Housing Needs. As such, he serves as an advocate for maintaining the rural character and natural features of the Blue Ridge Mountains as well as Western Loudoun, which is occupies approximately 3/5 of the entire in County. In addition, he has written position papers and lobbied on behalf of FBRM on issues concerning planning, zoning, performance standards for rural economy uses, subdivision design standards, and a leader in opposition to the AT&T data center on the Short Hill.
CELEBRATIONS, OUTREACH, AND COMMUNICATIONS COMMITTEE
Rebekka Prinz, Chairperson
Mission: To plan, coordinate and publicize events and activities that engage a variety of people from across the region in celebrating, preserving, and enhancing the Blue Ridge Mountains. To avail opportunities to introduce our mission and our work to a variety of audiences. To produce written and electronic materials on behalf of the organization and its activities as needed.
MEMBERSHIP AND DEVELOPMENT COMMITTEE
Larry Malone, Chairperson
Mission: to expand the number of members for the purpose of ensuring that Friends maintains a strong financial base, providing volunteers for special projects and raising awareness of the need to safeguard the treasured Blue Ridge Mountains. To cultivate and seek major gifts from individuals, corporations, and foundations as needed for special projects.
Patric Copeland, Chairperson
Mission: to highlight the value of stewardship practices in conserving the health of the Blue Ridge mountains to members and the public through Action, Education, and Outreach; and to help raise funds to assist members with on the ground stewardship projects.
Carole Napolitano, Chairperson
Mission: to promote awareness and appreciation of the importance of audiences through programs and initiatives that feature the mountains diverse resource and historic/cultural significance

domain: geography


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American community gardening association builds community by increasing and enhancing community gardening and greening across the united states and canada. As a 12-unit package, the tower garden community garden is perfect for schools, restaurants, nonprofits, and other community applications. There are three community gardens operated by bellingham parks & recreation the gardens contain a total of 195 plots community garden plots measure 10 feet by 20 feet water service, compost bins, rock bins and bulletin. The community garden plots are open to the public and offer a great space to practice organic gardening the community garden is located on a quarter-acre on the.
Start a community garden in your neighborhood don't have enough room or sun to grow what you like at home consider renting a plot in a community garden. Community gardens are great for those with little space read here for more community garden information and what to plant in a community garden plot click this article to learn more. Willowgate community garden the willowgate community garden is located at the end of andsbury avenue in mountain view and offers 92 individual plots the garden is open to adult mountain view residents and current city employees that must adhere to the willowgate community garden policies. The coralville community gardens offer a place for citizens to lease a plot of land to plant, garden, and grow their own fresh produce, herbs, and flowers.
Some influential [clarification needed] community gardens, such as the la plaza cultural community garden in lower manhattan in new york city, and the peralta garden in berkeley, california, inspired by architect and community garden visionary karl linn, are gathering places for neighbors and showcases for art and ecological awareness, with. Community gardening community gardens are plots of land, usually in urban areas, that are rented by individuals or groups for private gardens or are for the benefit of the people caring for the garden dig into these resources to learn about healthy, local food. Community gardens community gardens are collaborative projects on shared open spaces where participants share in the maintenance and products of the garden, including healthful and affordable fresh fruits and vegetables. • community gardens foster the development of a community identity and spirit • community gardens bring people together from a wide variety of backgrounds (age, race, culture, social class) • community gardens build community leaders.
Springwood community garden, springwood, new south wales 557 likes 1 talking about this 2 were here a community garden in springwood run by and for. Urban harvest supports more than 100 community gardens throughout houston neighborhood and allotment gardens provide an opportunity for neighbors to grow nutritious food as a community and create an urban oasis for the neighborhood. Get involved and try out your green thumb with one of portland's community garden locations.
Become a co-op gardener at desert botanical's onsite community garden and learn best practices of growing vegetables in the low desert climate. The kccg mission is to empower and inspire low-income households, community groups, and schools in the kansas city metropolitan area to. Find the right spot for your community garden, and you can potentially boost property values while saving money on produce.
Starting a community garden steps to organizing your community garden 1 get your neighbors involved there is a lot of work involved in starting a new garden. Most community gardens are designed for growing food, vegetables and fruits community vegetable gardens may be in individual or family plots and often support food banks, church missions or shelters some gardens are based on a fee structure where you rent a garden space and manage your own plot. Boise city recognizes community gardens as a valuable recreational activity that contribute to community development, environmental awareness, and positive social interacation, and that support increased local food production and food security. Starting a community garden this fact sheet is designed to give many different groups the basic information they need to get their gardening project off the ground.

domain: hobby


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A senior Labour MP has called for Parliament to have the right to send back the Government’s Brexit plans as inadequate – before any vote on starting Britain’s EU exit.
Hilary Benn, the new chairman of the Commons Brexit committee, said MPs should be able to tell ministers to “change this or do that” before a decision on triggering Article 50.
Mr Benn said such a timetable would prevent critics claiming some MPs were attempting to block Brexit, because it would not be a vote on whether to invoke the key article – and start withdrawal.
He said: “It’s not a vote on Article 50 – I think Parliament would seek to have a vote on the negotiating plan, because they are two different things.”
Speaking to the BBC’s Andrew Marr programme, Mr Benn added: “The Government might need to come back and say ‘alright, we have had a think about it and we are going to change this or do that’."
The call from the MP now in charge of scrutinising Brexit will infuriate Theresa May, who has insisted Parliament will not be given either a vote or a “running commentary” on her exit strategy.
It underlines what MPs believe is their growing strength in the tussle to influence that strategy – even before the High Court ruling on whether the Government can legally act alone on Article 50.
Asked if the Prime Minister would have to call a general election if MPs vetoed her negotiating plan, Mr Benn said that was “not in the hands of me or the select committee".
He also demanded that the Government announce whether it will seek a transitional arrangement for businesses after Brexit, if no trade deal can be thrashed out by the date of departure.
Last week, Brexit Secretary David Davis became the first cabinet minister to admit that British companies face a damaging “cliff edge” of high tariffs if a new deal cannot be struck in time.
Mr Benn said: “The importance of a transitional arrangement is it would offer some confidence to business.”
Away from economics, other key issues included whether Britain will remain a member of Europol, or continue to enforce the EU-wide arrest warrant, he said.
Ministers must decide by the end of this year whether to accept a new, expanded remit for Europol agreed by the 28 member states after the Paris and Brussels terror attacks.
If they do, the UK police and intelligence services – which strongly favour the move – will continue to have full access to the law enforcement agency’s databases and services.
However, it would anger some Brexit-supporting Tory MPs, because the UK would have to pay budget contributions to the EU and accept a role for the European Court of Justice in resolving disputes.
Many MPs are demanding a full Commons debate and vote on Europol within the next month, as the first big test of what Brexit means.
Asked about Mr Benn’s demands, Transport Secretary and Brexit supporter Chris Grayling repeated that the Government would not be “laying all its cards on the table”.
He told Mr Marr: “We will be informing Parliament as much as we can, but the national interest has to come first.”Reuse content

domain: law


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Some people decorate an Easter tree during the festivities and others prepare egg-citing Easter egg hunts for the little ones – no matter which camp you fall into, these small, hanging, wooden eggs are the perfect addition to your celebrations.
This set of four wooden eggs have been painted with stunning floral designs, in the most vibrant of colours, and come with dainty ribbon attached, so that you can hang them wherever you desire. Measuring just 6cm, these tasteful little eggs are an investment as they will last you year after year of seasonal fun.
- Set of 4
- 6cm Floral (Bluebell, Daffodil, Daisy & Bluebell, Multicoloured)
- Other colourways available

domain: design


Welcome to the Portneuf Greenway Foundation
The Portneuf Greenway Foundation’s mission is to create a network of paved bicycle and pedestrian trails throughout the greater Pocatello Chubbuck area to enhance the quality of life for residents and visitors by establishing and improving the Portneuf Greenway as a community resource. The foundation is a 503(c) organization established in 1992 and is governed by a volunteer board of directors. The Foundation has no paid employees and receives no direct funding from the City of Pocatello or Chubbuck for public facilities.
Development of the Portneuf Greenway is guided by the Portneuf Greenway Master Plan and a supporting Capital Investment Plan. Though the Greenway Foundation focused on establishing trails along the Portneuf River initially, the broader vision is to connect a comprehensive trail system throughout the Pocatello and Chubbuck communities respectively. Several trails have recently been established along the I-15 corridor, the South Bannock Overpass, as well as in and around the Edson Fichter Nature Area in South Pocatello. Since 2014, the Portneuf Greenway Foundation has been the recipient of approximately $7.5 million in grants, public and private contributions, gifts and in-kind construction.


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President Joe Biden indicated that his administration is open to further action on student debt relief in a meeting Monday with the Congressional Hispanic Caucus, according to a report from The Washington Post.
White House Press Secretary Jen Psaki confirmed the president’s comments in a briefing Tuesday, stating that he “is looking at other executive authority options he has to bring relief to people who have student loans” and will make a decision before the current pause on loans ends Aug. 31.
During Monday’s meeting, the president was asked by Rep. Tony Cárdenas to extend the current moratorium on loan payments, as well as cancel $10,000 worth of student loans per person via executive order, the report says. He was “incredibly positive” to the suggestions, Rep. Cardenas told the Post. Biden also implied that he wanted take action sooner rather than later to cancel some student loan debt when pressed by other lawmakers, the Post reported.
There is a total of $1.75 trillion in outstanding student loan debt in the US, a number that has more than tripled in the last 15 years. This is thesince the beginning of the COVID-19 pandemic, the last three of which were ordered by the Biden administration.
The expanded moratorium on loan payments is helping 41 million Americans save a collective $5 billion, according to the Department of Education. Over the past year, the Biden administration has taken other actions to help borrowers, such asto correct experienced by some borrowers, many of whom should have had their loans forgiven already but in many cases never received any debt relief.
Monday’s meeting with Democratic lawmakers signaled that the president is ready to head down a path to further student loan forgiveness, telling those present at the meeting they would be “very happy” with what he planned to do next, according to the Post.
The White House did immediately respond to a request for comment.


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A new study has found that men who delay having children are more likely to have “geekier” sons. The “Geek Index” devised by the King's College London was tested on kids of older fathers and it found that these kids were more intelligent and focused and less bothered about being included and fitting in. The mothers did not seem to have an impact and daughters too did not have an impact from being born to older fathers says the study.
Image Credit: Arina P Habich / Shutterstock
Delayed parenthood is the norm today with careers being on line at younger ages. Scientists believe this could lead to production of more geniuses in the society. Delayed parenthood for women as well has men has been often studied with more bad news than good.
Delaying parenthood has been linked to genetic defects in the baby, autism and several other congenital problems. This is mainly because the older the sperms (from the father) and the ova (from the mother) get, more they are likely to develop genetic errors.
In addition the risk of miscarriages and infertility also rises with age. This is probably the first that said anything good about delayed fatherhood say researchers.
For this study the researchers looked at 15,000 twins who were a part of another large study. Their Geek index was used to check on the “geekiness” of the kids at the age of 12. The points tested included ability to focus on a topic, non-verbal IQ and social aloofness or lack of concern about not fitting in.
Those that scored high on the Geek Index did better at school especially in science, mathematics, technology and engineering. These high scorers were linked to higher paternal age and the connection was found to be robust.
Researchers explain that the possible explanations for this connection could be the fact that these kids have geekier fathers.
Typically, so called "geeks" or ones who are more intelligent and socially aloof, tend to start their family late and may be passing on their traits to their male children.
These older fathers are also ones that are financially more stable and probably are providing a better education and guidance to their sons explained researchers.
On a cellular level, researchers say that there may be changes in the sperm at older ages that affect development.
Dr Magdalena Janecka, from King's College London, lead researcher on the team said that the father’s age may not be the only deciding factor while planning to have children. There may be several risks involved with delayed parenthood.
Also the researchers are unable to explain why the girls did not show similar outcomes. They speculate that their test or Geek Index could be flawed to test geekiness in girls and could be missing the important differences among girls of older fathers compared to those of younger fathers.
Researchers mention that there is a thin line between geeks and autism and a slightest change in the two could tip the balance towards autism. This study according to them was to ascertain the link between “advanced paternal age, autism and talent”.
The study was published this week in the journal Translational Psychiatry titled “Advantageous developmental outcomes of advancing paternal age”.


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Universities and Their Role in Economic Development
By Alejandra Guzman
Click aqui para español- >Las universidades y su impacto en el desarrollo económico
It is hard to think about economic development without considering the role universities play. Academia, the private sector, and other financial stakeholders rely on one another to create economic opportunities. Leveraging talent, innovation, and location with the interconnectedness of each of these elements are critical to creating economic opportunities. Universities also play a crucial role in shaping the policies of a region and addressing the needs of society to boost the economic, social, and cultural development of communities. From a place perspective, higher education institutions contribute to their communities’ overall aesthetic and quality of life through their campuses and sites.
Many universities worldwide have evaluated their campuses and have aimed to provide living quarters for students and staff, offering high-quality public transportation and attractive commercial and cultural functions that enhance the quality of the location.
This quality of place serves their community and serves external stakeholders who seek to engage with universities expecting these institutions to address the needs of society, including fostering economic development.
University leaders understand these expectations, and many are already trying to strengthen university engagement with society by carefully considering the needs of the community for their evolution.
Two good international examples of universities that recognize stakeholder engagement and stimulates urban activity are the Tecnologico de Monterrey in Mexico and Bilgi University in Istanbul.
Bilgi University has followed a model of buying and restoring former industrial buildings in underdeveloped neighborhoods to provide adequate and affordable premises for its growing activities while giving a socio-economic boost to the surrounding city quarters.
A particular project that has garnered attention is the Santral project, involving a former power station. The rich cultural, political, and economic history of the site and Istanbul, more broadly, makes the success of this regenerating process impressive. Its design and use were carefully crafted to respect the heritage and needs of the community.
In Mexico, the Tecnologico de Monterrey has reimagined its urban footprint impact. This institution created Distrito Tec, an initiative that addressed a rapid outward expansion that ignited a low-density, resource-inefficient metropolitan area plagued by congestion and drug violence.
The university collaborated in designing a master plan for the evolution of the campus, which included 24 surrounding neighborhoods as part of a cohesive district. The urban transformation increased public and green space, pedestrian and cycling paths, and social cohesion through cultural and community programming.
New Orleans is home to a vast network of higher education institutions, including Tulane University, Xavier University of Louisiana, Loyola University New Orleans, LSU Health Sciences Center, University of Holy Cross, University of New Orleans, Dillard University, Southern University, Nunez Community College, and Delgado Community College. The contributions to the economic and community development that these institutions generate are tremendous and have a city, state, and national impact.
Let us celebrate and support our universities! They certainly play an essential role in our society.
VIVA NOLA JUNE-JULY 2021 You can support VIVA NOLA’s mission of connecting communities by donating here. Your support, in any amount, is very appreciated.

domain: economics


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Chan Sung Jung, popularly known as ‘The Korean Zombie,’ will need to find a new spot to train, at least temporarily.
Jung last took to the octagon against the current UFC featherweight champion Alex Volkanovski in April at UFC 273. Former division title holder Max Holloway was initially lined up for Volkanovski, but Jung was found as the replacement after Holloway was forced to withdraw from the bout.
Volkanovski handily dispatched Jung in the fourth round after dominating him throughout the contest.
The Korean Zombie forced to close gym after rain storm flooding
‘The Korean Zombie’ got back to the drawing board as he recovered from the damage sustained by his latest loss. His training will need to be put on a halt for now, as a natural mishap ruined his previous facilities. A rain storm ended up flooding his gym, which now needs to be repaired.
Jung shared the news on his Instagram account, writing: “I think I should close the gym for a while. I’ll have it restored as soon as possible. 😢 We will announce as soon as possible to operate. Thank you for your understanding.”
You can watch the video below.
It was not only Jung who suffered as the record rainfall caused deadly flooding in Seoul, killing at least eight people, according to CNN. He posted follow-up stories of the gym and it appeared that he had already started cleaning up the place. However, restoration work would remain still to get everything back in working condition.
Jung’s toughness and incredible durability made him a fan favorite. ‘The Korean Zombie’ hinted at retirement but eventually decided against it following the defeat to Volkanovski. He has been competing in the UFC for over a decade, having started his pro career in 2007 before making his debut in the promotion in 2011.


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Upcoming Workshop and Artist Talk with Orion Crook
Our Summer 2022 Artist-In-Residence Orion Crook will be guiding two special events at Chinkapin Craftstead. On Sunday, August 21, at 4:00 PM, the workshop "Healing Alongside Expressive Arts" will take place and explore the ways by which artistic expression can be a healing practice in one's life. This workshop will be interactive, and art supplies will be provided.
On Saturday, September 3, at 4:00 PM, Orion will host an Artist Talk that will be a deeper dive into their creative process and artistic perspectives.
All are cordially invited to participate in these events!

domain: artistic


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Apr 30, 2014 9:50 PM by Chief Meteorologist Bill Meck
We're entering the cooler phase of this complex storm system that has been on our weather maps since last week.
On Thursday we'll see a cloud sun mix with more clouds during the afternoon. A few stray showers can't be ruled out, but they'll be light and brief if you get one, but many of us won't. The highs will be cooler, only around 60 or so.
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Nonthermal emission from high-mass microquasar jets affected by orbital motion
Key Words.:X-rays: binaries - radiation mechanisms: nonthermal - stars: winds, outflows - stars: massive
Context:The stellar wind in high-mass microquasars should interact with the jet. This interaction, coupled with orbital motion, is expected to make the jet follow a helical, nonballistic trajectory. The jet energy dissipated by this interaction, through shocks for example, could lead to nonthermal activity on scales significantly larger than the system size.
Aims:We calculate the broadband emission from a jet affected by the impact of the stellar wind and orbital motion in a high-mass microquasar.
Methods:We employ a prescription for the helical trajectory of a jet in a system with a circular orbit. Subsequently, assuming electron acceleration at the onset of the helical jet region, we compute the spatial and energy distribution of these electrons, and their synchrotron and inverse Compton emission including gamma-ray absorption effects.
Results:For typical source parameters, significant radio, X- and gamma-ray luminosities are predicted. The scales on which the emission is produced may reduce, but not erase, orbital variability of the inverse Compton emission. The wind and orbital effects on the radio emission morphology could be studied using very long baseline interferometric techniques.
Conclusions:We predict significant broadband emission, modulated by orbital motion, from a helical jet in a high-mass microquasar. This emission may be hard to disentangle from radiation of the binary itself, although the light curve features, extended radio emission, and a moderate opacity to very high-energy gamma rays, could help to identify the contribution from an extended (helical) jet region.
High-mass microquasars (HMMQ) are X-ray binaries that host a massive star and a compact object (CO) from which jets are produced. The stellar wind can strongly influence the jet propagation, both because the jet has to propagate surrounded by wind material, and because the wind lateral impact may significantly bend the jet away from the star. Several authors have used numerical and analytical methods to study, on the scales of the binary, the interaction of HMMQ jets with stellar winds and their radiative consequences (e.g., Romero et al. 2003; Romero & Orellana 2005; Perucho & Bosch-Ramon 2008; Owocki et al. 2009; Araudo et al. 2009; Perucho et al. 2010; Perucho & Bosch-Ramon 2012; Yoon & Heinz 2015; Bosch-Ramon & Barkov 2016; Yoon et al. 2016).
On scales larger than the binary system, orbital motion should also affect the dynamics of the jet, making it follow a helical trajectory (e.g., Bosch-Ramon 2013; Bosch-Ramon & Barkov 2016). There are a few well-established microquasars in which evidence of a helical jet has been observed; for example, SS 433, 1E 1740.72942 and Cygnus X-3 (Abell & Margon 1979; Mioduszewski et al. 2001; Stirling et al. 2002; Miller-Jones et al. 2004; Luque-Escamilla et al. 2015; see also Sell et al. 2010 for the possible case of Circinus X-1). In the case of SS 433, the jet helical geometry likely originates in the accretion disk (e.g., Begelman et al. 2006); in the case of 1E 1740.72942, the system likely hosts a low-mass star and the role of its wind could be minor; in the case of Cygnus X-3, the apparent jet helical shape has an unclear origin. Bosch-Ramon & Barkov (2016) proposed that Cygnus X-1 and Cygnus X-3 could be affected by orbital motion and the stellar wind, although the uncertainties on the jet and wind properties make quantitative predictions difficult. Unlike the case of Cygnus X-3, no clear evidence of a helical or bent jet has yet been found for Cygnus X-1 (Stirling et al. 2001).
In this work we study the implications of the impact of the stellar wind and orbital motion for the nonthermal emission of a HMMQ, from radio to gamma rays. Using an analytical prescription for the jet dynamics based on the results of Bosch-Ramon & Barkov (2016), the nonthermal radiation from a helical jet (spectra, light curves, and morphology) is computed numerically, considering a leptonic model with synchrotron and inverse Compton (IC) emission.
The paper is organized as follows: In Sect. 2, the interaction between the stellar wind and the jet is described. The technical aspects of the model are explained in Sect. 3. The results of the calculations are presented in Sect. 4 and a discussion is provided in Sect. 5. Unless stated otherwise, the convention is used throughout the paper, with in cgs units.
2 Jet-wind interaction
The physical scenario considered in this work consists of a massive star with a strong stellar wind and an accreting CO from which two jets are launched in opposite directions perpendicular to the orbital plane. The binary has a relatively compact orbit, taken circular for simplicity, with a period of days and a separation of cm (). The luminosity of the star is taken to be erg s, and its temperature K (). The stellar wind is assumed to be spherically symmetric, with a mass-loss rate and a velocity of M yr and cm s, respectively (typical for O-type stars; e.g., Muijres et al. 2012). Such a system would have similar parameters to those of Cygnus X-1, although it would be significantly wider and with a weaker wind than Cygnus X-3 (but the adopted wind and jet momentum rate relation will be similar; see below).
The orbit is assumed to lie on the -plane, with the star at the center of coordinates. The CO would be on the -axis, orbiting the star counter clockwise, and the jet (counter jet) would initially point along (). The axes are defined in a frame corotating with the CO around the companion star. The jets are assumed to have a conical shape, with an initial half-opening angle rad . In this work, we do not need to adopt a specific value for , although to make our predictions qualitatively valid, it should be smaller than the jet deflection angle imposed by the wind impact (see below). We take an initial jet Lorentz factor of , although the final results are not sensitive to this parameter as long as the jet is strongly supersonic and mildly relativistic. The jet power is taken as erg s.
Figure 1 sketches the scenario under study. The jet goes through three stages, the first of which is not present in the figure: Initially, the jet moves perpendicularly to the orbital plane. Then, the wind impact produces an asymmetric recollimation shock on the jet, which gets inclined away from the star (stage 2). Further from the binary, the combined effect of the stellar wind and orbital motion leads to a (orbit-related) force that bends the already inclined jet, now against orbital motion (clockwise in Fig. 1). In this way, the jet becomes helical, with asymmetric shocks being expected because of the orbit-related force (stage 3). Here it is assumed that electrons are efficiently accelerated in those shocks, ascribed here to one specific point: the onset of the helical jet, which neglects the fact that acceleration may occur along the helical jet region. Relativistic protons may also be generated in those shocks, but their radiation efficiency would be much lower in general, and therefore they are not considered in our calculations (see e.g., Bosch-Ramon & Khangulyan 2009, for a discussion of the different electron and proton cooling timescales in HMMQ).
For the radiation calculations, a fraction of is injected in the form of nonthermal electrons right where the jet starts its helical path. This fraction is only constrained by , although the predicted luminosities are proportional to its value and easy to translate if a different fraction is adopted. Nevertheless, adopting does not require particularly efficient acceleration processes. The inclination of the system with respect to the line of sight of the observer, assumed to be at a reference distance of kpc, is characterized by the angle . The values for the different fixed parameters of our model are listed in Table 1.
|Star luminosity||erg s|
|Wind speed||cm s|
|Wind mass-loss rate||M yr|
|Jet luminosity||erg s|
|Initial jet Lorentz factor||2|
|Half-opening angle||0.1 rad|
|Nonthermal energy fraction|
|Effective flow velocity||cm s|
|Radial flow velocity||cm s|
|Distance to the observer||3 kpc|
|Radio interferometer resolution||FWHM||1 mas|
2.1 Wind impact: jet bending
Interaction between the stellar wind and the jet can lead to bending of the latter in the -axis direction (stage 2 above). This bending can be characterized by an angle with respect to the jet initial direction (i.e., the -axis; see Fig. 1). Following Bosch-Ramon & Barkov (2016) we introduce a nondimensional parameter, , which corresponds to the ratio between the wind momentum rate intercepted by the jet, and the jet momentum rate:
where is in units of M yr in the rightmost expression, is the stellar wind momentum rate, and is the jet momentum rate, which can be expressed in terms of , , and the initial jet velocity in units :
An approximate computation of the bending angle , with a discrepancy of less than 10% with respect to the numerical case, yields the following expression (for more details, see the Appendix in Bosch-Ramon & Barkov 2016):
For bending angles , the lateral impact of the stellar wind may produce a weak recollimation shock or a sound wave in the jet, and the large-scale jet evolution should not be strongly affected (although the role of instability growth may still be important; see, e.g., Perucho & Bosch-Ramon 2008; Perucho et al. 2010; Perucho & Bosch-Ramon 2012, under uniform and clumpy stellar winds). However, when is significantly larger than , a strong asymmetric recollimation shock is expected, with the jet substantially deviating from its initial direction. In such a case, the jet is likely to turn into a helical-shaped structure at larger scales (stage 3, above). Consequently, bending due to stellar wind impact becomes important for the jet evolution when .
2.2 Orbital effects: helical jet
The orbital motion of the system combined with a jet inclined by the stellar wind (stage 2) leads, through the orbit-related force, to a jet helical pattern. This effect becomes clearer for significant bending angles. Otherwise, for , the conical jet expansion will dominate the geometry of the resulting structure. We note that a helical pattern would be expected from an inclined jet even under ballistic jet propagation, but the presence of the stellar wind makes jet propagation nonballistic. Instability growth should also play a role, but here we consider its effects only phenomenologically through a slower jet flow, caused by the wind mass entrainment and hence deceleration associated to instabilities.
One can estimate the distance that a nonballistic jet travels in the -axis direction before acquiring a negative velocity -component, i.e., bending against the orbital motion. With the additional assumptions that the half-opening angle of the jet remains constant after being bent (see below), and that is much larger than the orbital separation, we get (see Bosch-Ramon & Barkov 2016, for the derivation of this expression):
where is the orbital angular velocity, with the normalization corresponding to a period of several days (e.g., rad s), and is a constant of , introduced to account for the specific details of the wind-jet interaction. Here we fix .
Knowing and , we can compute the height at which the jet starts forming the helical structure: . For the parameters given above, and following Eqs. (3) and (4), the location vector of the beginning of the helical structure is cm, with . We note that cm, as required. The distance from to the star is cm and to the CO is cm. The jet curvature due to orbital motion for distances smaller than is neglected, that is, .
The point (the -helical- jet base hereafter) is the position where nonthermal electrons are injected. The evolution of these electrons is followed from this point onwards along the helical jet assuming that no more significant electron acceleration happens further downstream in the jet111We note that as the jet propagation is nonballistic, (weak) acceleration regions may also exist all along the jet due to jet kinetic energy dissipation.. Electron acceleration may also happen closer to the binary system (see Sect. 5), but here we focus specifically on the nonthermal emission produced in the helical jet region.
From onwards along the jet, the stellar wind should have a very important dynamical role. As the jet becomes helical due to the presence of wind plus orbital motion, the former is also pushing the latter in the radial direction. Therefore, the radial velocity () of the jet flow may be as slow as the stellar wind itself, or higher if the shocked stellar wind is effectively accelerated radially by the jet. In addition, effects of wind entrainment are likely to affect the jet flow itself, slowing the latter down to an effective velocity . We adopt here and as phenomenological parameters that fulfill . They provide a simplified prescription for the helical jet geometry, defining the pitch of the helical jet trajectory. It is also assumed that this trajectory is confined to the conical surface, characterized, in the nonrotating frame, by the direction determined by the vector along the orbit in that frame (i.e., a ring traced by the points , plus the radial direction from the star), which should be a relatively good approximation as long as .
The half-opening angle of the helical jet flow () need not be constant, as the nonballistic nature of the jet trajectory, with weak-shock heating, rarefaction waves, wind (re)confinement, and mass-loading, may lead to (re)collimation or (re)widening of the helical jet, depending on the details of the jet and wind interaction. For simplicity, at this stage we assume . In addition, we also take cm s and cm s; this is somewhat arbitrary, but except for the radio morphology (see Sect. 5) their actual values do not qualitatively change the results. Hydrodynamical simulations are required to properly characterize , , , the role of instability growth, mass-loading, and so on. Nevertheless, we consider our dynamical model realistic on scales of a few , as large-scale perturbations should grow up to a size to disrupt the helical structure.
3 Model description
We use a semi-analytical code to compute the energy and spatial distribution of the accelerated electrons. As the orbital period is significantly longer than the crossing time of the helical jet length (), the nonthermal electrons are assumed to be in the steady state at each orbital phase.
3.1 Energy losses
Analytical expressions for the energy losses are used in this work. For synchrotron cooling, assuming, for simplicity, an isotropic magnetic field in the flow frame, one obtains, in cgs units (Longair 1981):
where is the Thomson cross-section, , and is the Lorentz factor of an electron with energy . The magnetic field at the jet base is parametrized through the ratio of magnetic pressure to stellar photon energy density, , as
This way of normalizing allows an easy comparison between the expected luminosity of synchrotron and IC emission; for IC in the Thomson regime, the two processes contribute similarly for electrons of the same energy if . However, for electrons of energy (with being the Boltzmann constant), which scatter photons in the IC Klein-Nishina regime, already leads to global strong synchrotron dominance, which is corroborated by our calculations. One can relate with the ratio of magnetic pressure to jet energy density () for the same via: ( for the values adopted here).
Losses due to IC are computed as in Khangulyan et al. (2014) for an isotropic electron population embedded in the stellar photon field taken as a black body of temperature . This expression is valid in both the Thomson and the Klein-Nishina regimes and has an accuracy of :
with being the radius of the star, the distance from the star to the emitter, , and
For a conical jet, adiabatic losses are
where is the jet expansion velocity and is the helical jet radius.
The total energy-loss rate is
3.2 Electron distribution
The nonthermal electrons are injected in the jet base with an energy distribution that follows a power law of index -2, typical for efficient nonthermal sources (and for acceleration in nonrelativistic strong shocks; Drury 1983), plus a cutoff at high energies set by energy and escape losses:
We note that a much steeper would mean inefficient electron acceleration, whereas a much harder one would imply exceptionally efficient acceleration in which most of energy is in the highest-energy electrons.
The normalization of the electron injection is taken as a fraction of the jet power available for the acceleration of nonthermal electrons, :
The value of is fixed here to 1 MeV for simplicity, although a very high , greater than GeV for example, would affect the more compact radio emission. The value of is obtained from electron acceleration constraints.
Electrons are accelerated gaining energy at a rate , where is the acceleration efficiency, and the electron charge. We take , which would correspond, for example, to acceleration by a high-velocity (nonrelativistic) shock under Bohm diffusion (Drury 1983). Low acceleration efficiencies would reduce the maximum energy of synchrotron photons, for which the photon energy is , much more than that of IC photons, produced in the Klein-Nishina regime at the highest spectral end, for which (for IC in Thomson: ).
Equating yields the maximum energy that electrons can reach in the accelerator (at ): . However, electrons can diffuse away from the accelerator before they reach . Therefore, the diffusion timescale, , is also to be compared with the acceleration timescale, , where is the characteristic jet base radius, and is the diffusion coefficient assuming it proceeds in the Bohm regime. This gives a maximum energy value ; for a larger diffusion coefficient (still ), . The value is obtained as the smallest among and , whereas can be taken as several times .
To compute the electron energy distribution along the jet, the latter is divided in cylindrical segments with increasing radius. The segment lengths are determined (with some exception; see below) by multiplied by one fifth of the local shortest cooling time, which is derived from . In this way, the energy and spatial evolution of the fastest evolving electrons is reasonably well sampled. The magnetic field is assumed to be mostly perpendicular to the flow motion, typical for jets far from their origin, and therefore under frozen conditions and constant . Each individual jet division is treated as a homogeneous emitter, which in the worse case is correct within a % error (spatial scales grow segment by segment by a factor , where is the number of segments).
For , synchrotron cooling times become very short (, with being the advection timescale), and the large makes calculations very long. In those extreme cases, we have adopted an approximation which consists in limiting and then introducing a correction factor, , to the injected population at the first segment. This simplified approach can overestimate the high energy part of the electron distribution by a factor around two, but speeds up calculations by several orders of magnitude for extreme cases. Nevertheless, we indicate that is too high, as in the region of interest the jet power is likely largely dominated by kinetic energy, and is considered here for illustrative purposes only.
To find the energy evolution up to a given segment, one computes the initial energy that electrons of energy had when they were injected at the jet base. This is done iteratively by making small time steps back in time (and in space) to sample the energy evolution of electrons backwards from a given segment:
Here, is the energy that an electron had at a time , and is the electron energy at time . We note that due to the negative sign of . The linear approximation used in Eq. (13) is only valid as long as .
Once is known, the electron energy distribution at the jet base, , of a segment k with length , is computed as
with (if small enough; otherwise ). The electron energy distribution at a segment k is computed from the distribution when at the segment k-1:
where and are energies related by Eq. (13) in segments k and k-1, respectively222We note that Eq. (15) should be corrected for segment length and velocity if they are not constant.. By applying this procedure down to the jet base, one gets the general expression for the electron energy distribution at each jet segment:
keeping in mind that and .
3.3 Emission of radiation
The power per photon energy unit radiated by an electron of energy via synchrotron emission is computed following (Pacholczyk 1970)
where is the pitch angle between the electron velocity and vectors, and , with being the characteristic synchrotron photon energy defined as
The geometry of is not well known, so an isotropic distribution in the fluid frame is assumed, taking for simplicity . The synchrotron spectral energy distribution (SED) for an isotropic population of electrons with distribution is:
The IC emission is computed considering that relativistic electrons interact with a beam of photons with energy . The IC kernel for an angle with respect to the initial beam direction is (Aharonian & Atoyan 1981):
where , , and can vary in the limits . The (apparent) IC SED at a given direction is obtained by convolving Eq. (21) with the electron energy distribution and the energy distribution density of stellar photons :
Target photons other than those of stellar origin, like those coming from an accretion disk, are unimportant for the jet regions studied in this work. Synchrotron self-Compton is also negligible even when one assumes that most of the nonthermal energy is released as synchrotron radiation.
3.4 Absorption of radiation
The main absorption mechanism considered in this work is electron-positron pair production from gamma rays interacting with stellar photons. The cross section for this process is (Gould & Schréder 1967)
and are the energies of the high-energy and stellar photons, respectively, and is the angle between their propagation directions.
The optical depth of gamma-ray absorption is (Gould & Schréder 1967)
where is the distance to the observer covered by the gamma ray, and is the minimum energy of the gamma rays absorbed by the target stellar photons.
For the cases studied here, synchrotron self-absorption is estimated in radio by computing the optically thick-to-optically thin transition frequency (e.g., Bosch-Ramon 2009), and is found to be negligible in general; it has therefore not been included in the calculations. Free-free radio absorption in the stellar wind is also negligible at the scales of the emitting region. Nonthermal ultraviolet (UV) photons are also strongly absorbed on their way to the observer, but we have not included this effect as UV photons from the star would be largely dominant in any case. In a very compact system with a very powerful stellar wind, such as, for example, Cygnus X-3, radio absorption could still be an issue at a distance from the binary, although we defer specific source studies for future work.
The results are obtained using the parameter values given in Table 1, together with the sets of values presented in Table 2 for , the orbital phase , and , whose variations have strong effects on the nonthermal emission. Considering the free parameters, the electron energy distribution is affected only by , whereas SEDs, light curves, and the emitter geometry are also affected by and . Most SEDs are calculated for as a typical example, which corresponds to one of the orbit nodes. Varying , we also compute some SEDs and IC light curves to illustrate orbital variations of this component. A comparison of SEDs and light curves is done between the extended and the point-like (one-zone) emitter, to check which features arise when an extended (helical) jet is considered. Finally, maps at 5 GHz are computed to illustrate the expected radio morphologies from a helical jet.
4.1 Nonthermal electrons
The electron energy distribution for the jet333The jet and counter-jet electron energy distributions are equal in our model., to emphasize the energy content at different energy scales, is shown in Fig. 2 for and 1, and up to three different jet lengths starting from : , and (whole jet). As seen in the figure, a significant fraction of electrons below GeV survive beyond , and for the lowest , TeV electrons can also reach a larger distance from the binary (see also, e.g., Khangulyan et al. 2008). As expected, the energy distribution is steep for electron energies dominated by synchrotron and Thomson IC losses. When IC dominates, the SED becomes harder at GeV because of the Thomson-to-Klein-Nishina transition of the electron distribution, getting steeper again only at the highest energies due to synchrotron losses (and the effect of ).
4.2 Spectral energy distribution
Figure 3 shows the SEDs of the synchrotron and the IC emission for the same cases studied in Fig. 2, showing now within each panel the jet and the counter-jet contributions separately. An inclination of is adopted, and . As expected from the severe drop in radiation efficiencies, the contribution to the emission of the regions beyond is minor for all the cases studied, although radio emission is still non-negligible beyond that distance, as seen in Sect. 4.5. It is worth noting that most of the IC radiation comes from the counter-jet because of the larger IC -values. Doppler boosting is negligible for the adopted -value and is not included.
The effect of the magnetic field on the synchrotron and IC SEDs is shown in Fig. 4 for and , and for the jet and the counter-jet separately. As expected, the synchrotron to IC luminosity ratio depends strongly on . Figure 4 also shows the effect of gamma-ray absorption (stronger for than for ), which is quite modest given the relatively large distances from the star and the -value considered in this plot.
Figure 5 shows the effect of the orbital phase on the IC spectrum. With and , the SEDs for and are plotted. For , which corresponds to the CO superior conjunction (i.e., the CO is behind the star), there is a drop of up to five orders of magnitude in the counter-jet emission above 10 GeV due to gamma-ray absorption, which makes the jet dominate the radiation output in this range, effectively smoothing the overall impact of gamma-ray absorption for this orbital phase.
4.3 Light curve
Figure 6 shows the IC light curves for . The peak around and GeV for is explained by the larger IC -angles, and the small dip for manifests some level of gamma-ray absorption, which starts at GeV in a relatively hard IC SED (see Fig. 5). For energies GeV, absorption has a very strong impact on the fluxes by a factor of several, although the jet component smoothens somewhat the light curve around (superior conjunction of the CO) because of reduced gamma-ray absorption due to a smaller -value (see Fig. 5). On the other hand, the counter-jet still leads to significant IC fluxes around (inferior conjunction; see Fig. 5), unlike an emitter located very close to the CO, which would lead to stronger differences in flux.
4.4 Extended versus one-zone emitter
Figure 7 shows a comparison between the SEDs of an extended (helical) jet and a one-zone emitter, for the jet and the counter-jet, for , , and . The one-zone emitter is assumed to be just one segment located at and of length , which sets the electron escape time. Because of fast radiation losses, the one-zone approximation works well in the high-energy part of the synchrotron and IC SEDs, as expected. Qualitatively, the extended and the one-zone emitters look quite similar, although differences of up to a factor of 2 are seen, mainly but not only in the jet synchrotron and IC components at low energies, as low-energy electrons escaped from the one-zone region are still radiatively relevant. We note that inaccurate source knowledge and model simplifications imply systematic uncertainties likely larger than a factor of 2, which means that the SED alone cannot help to discriminate a helical jet model from that of a one-zone emitter.
Figure 8 compares the light curves of an extended and a one-zone emitter in the cases presented in Fig. 6. The fluxes are larger (lower) for the extended emitter for GeV ( GeV), and are symmetric around . The different behavior between the two energy bands is caused by the fact that electrons emitting GeV photons via IC reach farther from the star than those emitting GeV photons (see Sect. 4.1), both for the counter-jet and the jet, decreasing the IC flux as they meet a more diluted target photon field. We note that for higher jet powers, the helical jet would start further away (see Eqs. 1 and 4), in which case the light curve would become asymmetric for the extended jet.
4.5 Radio emission
Radio sky maps at 5 GHz for and different orbital phases are shown in Figs. 9 and 10 for = 30 and = 60, respectively. These maps are obtained following three steps: first, the helical jet structure is projected into the plane of the sky. Subsequently, the emission from each segment is convolved with a Gaussian with standard deviation to approximately distribute the emission over the actual sky-projected area of each segment. Finally, this emission is convolved again with a Gaussian with FWHM = 1 mas in order to mimic the response of a radio, very long baseline interferometer (see, e.g., Walker 1995, for a VLBA description). With the sensitivity of current instrumentation, typically of a few tens of Jy/beam, the extended emission could be resolved, but only from the parts of the jet that are relatively close to its base. The bending of the jet appears more dramatic the smaller the inclination due to projection effects. The total received flux for each map is 7.4 mJy. As the flux increases proportionally to , one could detect the jet up to larger distances for higher . To illustrate this, Fig. 11 shows a comparison between two sky maps with different nonthermal energy fractions, and . We note that the radio fluxes also depend on as .
5 Summary and discussion
As argued by Bosch-Ramon & Barkov (2016), a nonballistic helical jet region is the likely outcome of a HMMQ jet interacting with the stellar wind under the effect of orbital motion. In the present work, we have shown that such a region is predicted to produce significant fluxes from radio to gamma rays if erg s, for a source at a few kiloparsecs. These significant fluxes are explained by the high synchrotron and IC efficiencies at the helical jet onset location, , for typical HMMQ -values. Since realistic -values are expected to be well below equipartition with the radiation field, the IC component is likely to dominate the nonthermal emission, peaking around 10 GeV. Specific gamma-ray light curve features are also predicted: a non-negligible impact of gamma-ray absorption, combined with angular effects for this process and IC. Peculiar changing radio morphologies, which can trace the jet helical structure, are expected as well.
We note that hydrodynamical instabilities and wind-jet mixing make our results mostly valid for the inner helical jet region, say up to a few . Beyond that point, the jet helical geometry is likely to become blurred, eventually turning into a bipolar, relatively wide, and collimated supersonic outflow; a mixture of jet and wind material. Although the flow may still be mildly relativistic for very energetic ejections, in general the resulting ”jet” is expected to be much faster than the stellar wind, but nonrelativistic.
Our results are based on a number of strong simplifications, in particular regarding the stability of the helical jet. Therefore, detailed numerical simulations of the jet-wind interaction on middle to large scales are necessary for more accurate predictions. Nevertheless, despite the simplifications adopted, the main features of the scenario are expected to be rather robust, at least at a semi-quantitative level. These are: non-negligible fluxes; specific light curves characterized by the value of , the interplay of jet and counter-jet emission, and angular IC and gamma-ray absorption effects; and curved jet radio morphologies with characteristic orbital evolution. This is so because the first- or even zeroth-order level of the dynamical, radiative, and geometrical effects involved are taken into account in our calculations.
Two important system parameters, eccentricity and , have been assumed constant in our calculations. Despite being difficult to ascertain the impact of eccentricity in a high-mass microquasar without numerical calculations, simulations of pulsar-star wind colliding in eccentric binaries (Barkov & Bosch-Ramon 2016; Bosch-Ramon et al. 2017) suggest that the effect of eccentricity should be important only for rather eccentric binaries. In that case, the nature of the interaction structure may not be helical at all, being not only strongly asymmetric, and inclined towards the apastron side of the orbit, but also likely much more sensitive to disruption. The value of , and thus , may also change. This would leave the helical jet geometry unaffected: both the helical vertical step and are . On the other hand, the luminosity would change as except for emission produced under the fast radiative cooling regime of electrons (in our setup the highest-energy end of the synchrotron and IC emission), which is independent of . The helical jet radiation in a very wide system would be hardly detectable unless the flow is slow, which allows electrons to radiate more energy. On the other hand, in a very compact system, radio emission would be hard to resolve for a slow helical jet flow, as the source would be too small.
The emission on the scales of the binary, produced for instance by jet internal shocks or by the first wind-induced recollimation shock in the jet (stage 2), could be important. In which case: (i) assuming that the same nonthermal luminosity is injected in both regions, the radio emission from the binary scales would be strongly absorbed via synchrotron self-absorption and wind free-free absorption; and (ii) the X- and gamma-ray emission would be at a similar level if produced in the fast radiation cooling regime, and at a higher level otherwise because of the higher -value and IC-target density. Gamma-ray absorption could however strongly attenuate the gamma-ray luminosity GeV for most of the orbit. Therefore, the helical jet could contribute significantly to the overall nonthermal radiation of HMMQ, and particularly in radio and GeV, even if electrons are also accelerated closer to the jet base. This was the main motivation for this work: to perform a first exploration of specific radiation features of the helical jet region, so that it could be disentangled from the other emitting sites. For the HMMQ Cygnus X-1 and Cygnus X-3, their uncertain wind and jet parameters make it difficult to make concrete predictions; for example, a non-ballistic jet region may not form at all (see Yoon et al. 2016; Bosch-Ramon & Barkov 2016, and references therein), and an individual detailed source analysis is out of the scope of this work. In spite of this, our findings are not in contradiction with the radio morphology and the gamma-ray light curves of these sources (e.g., Stirling et al. 2001; Mioduszewski et al. 2001; Miller-Jones et al. 2004; Zanin et al. 2016; Zdziarski et al. 2018). Future detailed modeling together with deep, high-resolution radio observations and the high-energy light curves could provide hints of helical jet emission.
The wind-jet interaction in HMMQ resembles, to a significant extent, the wind-wind interaction in high-mass binaries hosting young pulsars. The latter sources are probably extended mostly on the orbital plane and along the orbit semi-major axis, whereas the bipolar helical-jet structure is focused mostly in a direction perpendicular to the orbit plane (Bosch-Ramon et al. 2015; Bosch-Ramon & Barkov 2016; Bosch-Ramon et al. 2017). Nevertheless, the interactions of the stellar wind with a relativistic pulsar wind or jet, on binary, middle, and large scales, share many qualitative properties, and this may mask a fundamentally different engine (accretion vs. a pulsar wind) when observing sources of yet unknown CO. These similarities are: extended radio structures with orbital evolution found at mas scales; strong radio absorption on the binary scales; similar hydrodynamics, and therefore impact of instabilities, adiabatic losses, and Doppler boosting effects444The much higher energy per particle of shocked pulsar winds can lead to stronger Doppler boosting effects than in a HMMQ jet, although mass-loading smoothens this difference., for the shocked flows outside the binary region; and gamma-ray light curves strongly affected by IC and gamma-ray absorption angular effects, in a likely extended/multi-zone emitter. Radio observations, high-quality multiwavelength data, numerical simulations, and realistic radiation calculations (e.g., Aharonian et al. 2006; Perucho & Bosch-Ramon 2008; Albert et al. 2009; Fermi LAT Collaboration et al. 2009; Perucho et al. 2010; Moldón et al. 2011b, a, 2012; Perucho & Bosch-Ramon 2012; Bosch-Ramon et al. 2015; Dubus et al. 2015; Zanin et al. 2016; Yoon & Heinz 2015; Yoon et al. 2016; de la Cita et al. 2017; Bosch-Ramon et al. 2017; Wu et al. 2018; Barkov & Bosch-Ramon 2018) are therefore needed to characterize radiation scenarios in high-mass binaries with unknown CO, such that empirical observables can help to disentangle the CO nature.
Acknowledgements.We would like to thank the referee for a constructive and useful report that helped to improve the manuscript. We acknowledge support by the Spanish Ministerio de Economía y Competitividad (MINECO/FEDER, UE) under grants AYA2013-47447-C3-1-P and AYA2016-76012-C3-1-P, with partial support by the European Regional Development Fund (ERDF/FEDER), MDM-2014-0369 of ICCUB (Unidad de Excelencia ‘María de Maeztu’), and the Catalan DEC grant 2017 SGR 643. EM acknowledges support from MINECO through grant BES-2016-076342.
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Although at first he seemed like traditional zombie fodder, I actually became quite attached to Axel in The Walking Dead Season 3. Of course, I didn't expect him to survive, but I did think we'd see the ex-convict lead some kind of redemptive storyline. As it turns out he was unceremoniously shot in the noggin by the Governor.
Of course, I wasn't the only one to be disappointed with his departure. At the recent FandomFest event in Kentuncky, Lew Temple, who plays Axel, gave ComicBook.com his thoughts. He explained:
I adore Axel. I felt really proud with what we did with him, and there was more to do for Axel and with Axel. As me, Lew Temple, I'm going to hopefully go on and continue to work, but Axel is all done. I was disappointed to have him fall by the wayside.
However, there is a chance Axel will come back from the dead — but probably not as you'd expect. Temple explained that Axel could potentially return to our screens in a flashback:
I know that I've had conversations, and they've had conversations with me about the possibility of the prison riot, when it all went down, coming back to film that, a flashback scene if you will. I think they would have done better to do that if they had kept one of us to tell that story. But who knows? Maybe, they'll find that somehow or another.
Personally, I don't feel super-optimistic about this happening. Sure, it would be a cool scene to see, but with none of the prison survivors still around, it might not add a whole lot to Season 4's story.
What do you think? Would you like to see a prison riot flashback, or are you more concerned with what actually happens during Season 4? Let me know below.

domain: entertainment


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27 September 1918
- Day 1520 of the war
- The Australian Mounted Division in Palestine launches the Battle of Jisr Benat Yakub (the Bridge of Jacob’s Daughters) continuing their advance towards Damascus
- Edward Charles Mann receives letters of condolence following his son Charles William Joseph Mann’s death in France on 6 July 1918. The Late Corp Mann
- Allied troops in France begin an assault on the German Hindenburg Line. Fighting in the Battle of the Canal du Nord continues until 9 October.
This entry was posted on September 27th, 2018.

domain: history


So it turns out that the Senate is sllooooooooooooow walking some of Barack Obama’s final-year nominations in the banking field. Specifically, Sen. Richard Shelby of Alabama is pretty much sitting on thirteen nominations Obama has made, including two each for the Federal Reserve and Securities and Exchange Commission, and one they-can’t-do-work-without-this-guy appointment to the Export-Import Bank… hold on, hold on! Don’t start cheering yet! Finish reading the post first! Sen. Shelby’s delay means that these spots won’t be filled before mid-January at the earliest. Assuming that they’re filled then. Hard for Sen. Shelby to say, really. It’s not like he can foretell the future.
The WSJ – who is by the way a good deal more upset about this than I am, and probably you are, and almost certainly the average American voter is – noted that the Fed spots were being held up as part of the usual I will sit on these nominations until you do what you said you would strategy, noted a little waspishly that “[Shelby] has been more vague about why he is delaying the rest.” I’m not entirely sure why the WSJ is being so peeved over what’s regular Dizzy City business. Possibly because Senator Shelby isn’t going to be the idiot that the WSJ wants him to be and spell it all out for the cameras?
But let’s get to the actual reasons themselves. My assessment here is that Senator Shelby is (as the WSJ notes in the article) indeed keeping his upcoming contested primary in mind, and that he’s using this as a proxy in his fight with the White House over both reforming Dodd-Frank and getting tougher Iranian sanctions. …Good. I like to see Senators worried about their jobs. I also would like to see the messy kludge that is Dodd-Frank ‘fixed*;’ and goodness knows that the Iranian regime needs a good, solid dose of negative feedback.
But there’s another, perhaps even more relevant reason: [mc_name name=’Sen. Richard Shelby (R-AL)’ chamber=’senate’ mcid=’S000320′ ] may simply feel that the current President of the United States is a gormless nincompoop whose track record of past nominations has been sufficiently abysmal that keeping Barack Obama from confirming anybody else for the next year is a meritorious act of service for the Republic. But perhaps I am merely misjudging the entire situation; this might not be the Senator’s intent at all. It’s instead just a serendipitous result.
(Image via Shutterstock)
PS: Always praise a politician when they do something that you want them to do. Yes, even when they’re only doing what they were supposed to be doing, anyway. It’s Operant Conditioning 101: think of it as the civic equivalent of house-breaking a puppy…
*Yes, read that particular word any way that you like.


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Reduced price on books for November 2018!
The Milton Keynes Book of Days of the Great War by Marion Hill, now reduced to £5.00
Everybody has a story to tell – this engaging book resulting from the Great War Remembered MK Heritage Lottery funded project includes diaries, letters, photos, interview extracts and news clippings to tell the story of local people, their places and their time (1913 – 1919) in their own words.
From young teenage soldiers to housewives and charity fund-raisers, they coped with immense hardships and trauma often with humour, kindness and sometimes extraordinary courage.
We will remember them
Available now from our online shop, where many books are reduced price for November 2018


The another Florida football scandal is now bubbling a little more frantically in the north of the state, as reports emerge of Tallahassee police making threats towards the family of a woman who had accused Florida State University quarterback and elite Heisman Trophy candidate Jameis Winston of sexual assault. Also released today is a faculty member’s open letter detailing am almost-medieval litany of horrors and intimidation perpetrated by the school’s Athletic Department, the players and their handlers.
Those who can’t get enough of this tale might want to know there is plenty more to be had in this part of the world, And I might be able to dig up a few to view.
Attack of the Giant Leeches (1959) is the source of a lot of great dialogue, concepts and alibis that could be applied to this scandal or all sorts of other ones. This low-rent AIP picture was produced by Gene Corman, Roger’s brother, and stars Ken Clark, fresh off his appearance as Stewpot in South Pacific (1958). Moonshiners, sheriffs, Seminole legends, an electro soundtrack presaging Star Trek and references to Cape Canaveral ‘radiation’ are just some of the entertaining tidbits in this battle with the Avis of swamp mutants.
The Legend of Boggy Creek (1972) is a ‘true life’ story set a little farther east, in the swamps surrounding Texarkana, AK. A big drive-in hit, this one combines documentary-like good-ole-boy scenes with almost MOR musical paens to the ‘monster’ Travis Crabtree, written by screenwriter Earl E. Smith. The end credit song sounds as if the warbler is Willie Nelson, and a Herb Alpert-styled trumpeter occasionally pops in and out of the mixes.
Finally, Return of the Swamp Thing (1989) features Louis Jourdan (Gigi (1958)) as the evil Dr. Anton Arcane (Moreau wasn’t available), Heather Locklear as his daughter, and Sarah Douglas (Ursa from the Christopher Reeve Superman (1978)). Need anything more be said? At least it does put things into perspective.
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domain: biology


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