San Francisco, CA – On view at Crown Point Press is an exhibition of etchings by scientists and mathematicians, September 4 - October 27, 2015. We came across this set of beautiful etchings on Artsy depicting mathematical equations. We decided to reproduce them on Authorea, using our equation editor and some LaTeX. Here’s the result.

MLT These notes are mostly inspired from reading Cox & Giuli (“Principles of stellar structure”); some insights are from A.Maeder (“Physics, formation and evolution of rotating stars”) and Kippenhahn & Weigert (“Stellar Structure and Evolution”) Pressure Scale Height In hydrostatic equilibrium we can define the total pressure scale height, $\hp$, as -{\D r} \equiv {\hp} = {\p} where $\p$ is the total pressure ($ + $). The pressure scale height is a measure of the distance over which the pressure changes by an appreciable fraction of itself.

_This is the author’s version of the work. It is posted here by permission of the AAAS for personal use, not for redistribution. The definitive version was published in Science on Vol. 350 no. 6259 pp. 423-426 , DOI: 10.1126/science.aac6933_ Internal stellar magnetic fields are inaccessible to direct observations and little is known about their amplitude, geometry and evolution. We demonstrate that strong magnetic fields in the cores of red giant stars can be identified with asteroseismology. The fields can manifest themselves via depressed dipole stellar oscillation modes, which arises from a magnetic greenhouse effect that scatters and traps oscillation mode energy within the core of the star. The _Kepler_ satellite has observed a few dozen red giants with depressed dipole modes which we interpret as stars with strongly magnetized cores. We find field strengths larger than $\sim\! 10^5 \,{\rm G}$ may produce the observed depression, and in one case we infer a minimum core field strength of $\approx \! \! 10^7 \,{\rm G}$.

There is on average one planet orbiting every star in the Universe. Our Galaxy (the Milky Way) is an immense disk of gas and stars with a diameter of about 100 000 light years, hosting about 100 billion stars and, therefore, also about 100 billion planets. Take a deep breath. Now, it turns out the Milky Way is just one of 100 billion galaxies that populate our Universe, a colossal expanding stretch of spacetime with an age of 13.7 billion years. The math is trivial: There are about 10 000 000 000 000 000 000 000 = 10²² planets out there. This number is extremely large. Apparently larger than the number of grains of sand found in every beach and every desert on Earth. But how many of these planets host life? And in particular, how many planets host intelligent life we might be able to communicate with? RSVP and join us for our second official NEW YORK OPEN SCIENCE MEETUP. Check this blog post series if you wanna know more. This event is supported by Authorea.com, Minds.com and the Bitcoin Center NYC.

Friday June 26, 2016. Today is a great day for human rights. The Supreme Court of the United States has ruled that the Constitution guarantees a right to same-sex marriage. This decision reflects a shift in American public opinion: according to recent polls, 60% of Americans now support same-sex marriage. As a company devoted to promoting openness and collaboration, Authorea feels strongly this is an important step in the right direction. Obviously, sharing the ups and downs of life with another person is an immensely more important and complex task than writing a collaborative paper. Yet if we can draw a parallel, we might say that a useful measure of the progress of a society, and humankind in general, is its ability to share and care openly, together. That’s the way to unlock society’s true potential, and foster creativity and love. Happy writing. Happy loving. Authorea

Tens of thousands of innovators met in Austin, Texas last week to discuss emerging tech, science, and innovation. It was the Interactive portion of South by Southwest (SxSW). Authorea was there. Among many great events, the MIT Media Lab presented “SOLVE”, an initiative set to bring together the most gifted researchers and innovators to identify and tackle challenges where new thinking and emerging technologies have the potential to make the world a better place. SOLVE identified four main themes: Learn, Cure, Fuel, Make.

THE TIMES THEY ARE A-CHANGIN Science is going through a rapid phase of transformation. Two important trends are emerging: 1. Research is becoming more complex, requiring larger collaborations and bigger experiments. 2. Science and technology increasingly affect modern society. The first trend is easy to understand. Let’s think of the cumulative knowledge of humankind as a sphere. Scientists work at the surface and try to “push the boundary”. Discovery increases the volume of knowledge. As the sphere’s volume grows, so does its surface area. Therefore an ever increasing number of researchers is required to tessellate the expanding cutting-edge of science. Moreover, contrary to a few hundred years ago when the sphere of knowledge was so small that a single polymath could master large chunks of it, nowadays no human can understand the details of more than a few research topics. To capture the bigger picture and understand very complex research questions, collaborative efforts combining together a number of highly specific expertises are required.

Last Thursday, September 22nd, we held our 5th New York open science meetup (#opensciencenyc). Science journalists, Columbia faculty members, and enthusiasts from our open science meetup group came out to hear Dr. Stuart Firestein talk about ignorance in scientific research and why it is necessary and valuable (yes, you read that right).

Watch this paper in real time at authorea.com/nytm

NEW YORK – Last June, a dedicated global team of Ebola researchers began an ambitious project to track the virus using large-scale genome sequencing. Their research, which was written on the research platform Authorea and published June 18 in the journal Cell , reveals critical information about how the virus traveled and mutated over seven months of the recent Ebola outbreak. Today Authorea is pleased to announce that the working draft, data, workflows, and full edit history of the paper are available to the public for free on Authorea. This is the first time that such complete details have ever been released for a scientific paper. This release provides unprecedented transparency and detail, empowering students and researchers to review every change and edit to every word during the writing of this landmark research paper, using Authorea’s “History” feature. “When we planned this study, our team decided to make our work as open and transparent as possible, and writing the paper on Authorea is part of that,” said co-lead author Daniel Park. “We felt a moral imperative to put everything out there, especially in this kind of emergency situation.” “Authorea was founded to make researchers’ day-to-day tasks easier,” says Authorea co-founder and Harvard Research Associate Alberto Pepe. “We realized we were wasting time emailing around documents and data. So we built a website where everyone could write and edit in the same place.” But Authorea also supports a bigger goal: making science more open. The platform is free to use for open research. “We encourage scientists to publish their entire research process: writing, data, and discussion,” said Dr. Pepe. “The default stance is often to be closed, and we encourage more openness and transparency.” Researchers in life sciences and other fields often withhold their raw data for months before and even after publishing, according to recent surveys. This practice has questionable utility, as it slows the pace of research, makes it less reproducible, and erodes public trust in science. “Open access saves lives,” said Professor Peter Suber from the Harvard Office for Scholarly Communication and the Harvard Open Access Project, which were not involved with the Cell Ebola study. “Research saves lives, and when access is unaffordable or delayed, the access barriers put lives at risk. This is especially true in a crisis like Ebola where time is of the essence.”

Great news! We're happy to announce that Authorea is one of the winners of the NYC-Paris Business Exchange competition. We'll be opening an Authorea office in Paris in March 2016. C'est génial!       

The core rotation rates of massive stars have a substantial impact on the nature of core collapse supernovae and their compact remnants. We demonstrate that internal gravity waves (IGW), excited via envelope convection during a red supergiant phase or during vigorous late time burning phases, can have a significant impact on the rotation rate of the pre-SN core. In typical (10 M⊙ ≲ M ≲ 20 M⊙) supernova progenitors, IGW may substantially spin down the core, leading to iron core rotation periods $P_{\rm min,Fe} \gtrsim 50 \, {\rm s}$. Angular momentum (AM) conservation during the supernova would entail minimum NS rotation periods of $P_{\rm min,NS} \gtrsim 3 \, {\rm ms}$. In most cases, the combined effects of magnetic torques and IGW AM transport likely lead to substantially longer rotation periods. However, the stochastic influx of AM delivered by IGW during shell burning phases inevitably spin up a slowly rotating stellar core, leading to a maximum possible core rotation period. We estimate maximum iron core rotation periods of $P_{\rm max,Fe} \lesssim 10^4 \, {\rm s}$ in typical core collapse supernova progenitors, and a corresponding spin period of $P_{\rm max, NS} \lesssim 400 \, {\rm ms}$ for newborn neutron stars. This is comparable to the typical birth spin periods of most radio pulsars. Stochastic spin-up via IGW during shell O/Si burning may thus determine the initial rotation rate of most neutron stars. For a given progenitor, this theory predicts a Maxwellian distribution in pre-collapse core rotation frequency that is uncorrelated with the spin of the overlying envelope.

Scientists are busy people. We have deadlines to meet, meetings to attend, lectures to give. And OF COURSE WE NEED TO WRITE PAPERS, not only because we are excited to share our findings, but also because scientific papers are the currency of the academic world. Authorea was created by scientists and for scientists. The idea: improving the process of writing and sharing the results of research. While Authorea has big plans for the paper of the future, in this post I want to focus on the here and now. This is because when I talk about the platform with my colleagues, by far the most common question I get is “Why should I use Authorea to write my paper?” GREAT QUESTION! Here some highlights that should make you curious: 1. With Authorea, your paper is accessible from any computer anywhere in the world. 2. You can write it from your browser, no installations required. 3. You can write in rich text (wysiwyg) LaTeX or in markdown. 4. Your paper is also a beautiful web page. 5. Collaboration is made easy. Managing your co-authors is straightforward. 6. Authorea is version controlled. Again, no installations required. 7. Adding citations has never been easier. Believe me, you will never wanna go back. 8. You can include data and code in your paper. This allows for transparency and reproducibility of results. 9. Export to any journal format with just one click. 10. Powerful commenting system. For internal or even external review. Ok, If you got this far you deserve more than a list of fancy features, so here’s my personal experience and why I think you should start using Authorea. I switched to writing papers with Authorea about a year ago and I noticed a number of immediate improvements: first of all MY PAPERS GET WRITTEN FASTER. Then I noticed that I have NO NEED TO EXCHANGE EMAILS WITH COLLABORATORS concerning the paper. This is fantastic. All the action happens (and it’s logged) on Authorea, including discussions about revisions and suggestions for improvements. This said, I didn’t really expect the most important upturn. By getting rid of the overhead I previously considered necessary, unavoidable parts of the scientific writing process, something remarkable happened. I actually STARTED ENJOYING WRITING MORE! And I do not mean just publishing; I had experienced that joy before. The difference is I now cherish the time I spend putting my science into words. It might sound crazy, but Authorea did something amazing: it made me DISCOVER THE PLEASURE OF WRITING SCIENCE TOGETHER with my collaborators.

如果您正在寻找基于网页的 LaTex 编辑器,Authorea 应该是您一个不错的选择。Authorea 是一个强大的在线 LaTeX 编辑器,并拥有很多强大的功能,包括立即可用的模板,方便合作的工具,文档更改历史记录,聊天功能,自动创建参考文献,方便插入图像,链接,表格等。 Authorea 还支持多种文件格式,包括 LaTeX,HTML,Markdown 等等。索引页面的创建,导出文件为 PDF,在社交媒体上分享,支持的平台:基于网页的,支持所有主流浏览器。快速编辑,打开/关闭评论,字数统计,这些都是 Authorea 能够提供的一些主要功能。这也是为什么它能成为 LaTeX 最好的的编辑器之一,使你能方便地用你最喜欢的浏览器做 LaTeX 编辑。Authorea 使得插入数学公式,图像和表格变得非常简单。总而言之,这些功能使得 Authorea 是一款简单易用的 LaTeX 编辑工具,你不需要花费很长时间就能学会使它。主要功能:非常容易插入图像,数学公式,表格和其它对象,合作,引用文章,自动创建参考文献,评论功能,可互动的图像,可插入 Ipython/Jupyter 文本。支持的平台:基于网页的,支持所有主流浏览器。

Asteroseismology of 1.0 − 2.0M⊙ red giants by the _Kepler_ satellite has enabled the first definitive measurements of interior rotation in both first ascent red giant branch (RGB) stars and those on the Helium burning clump. The inferred rotation rates are 10 − 30 days for the ≈0.2M⊙ He degenerate cores on the RGB and 30 − 100 days for the He burning core in a clump star. Using the MESA code we calculate state-of-the-art stellar evolution models of low mass rotating stars from the zero-age main sequence to the cooling white dwarf (WD) stage. We include transport of angular momentum due to rotationally induced instabilities and circulations, as well as magnetic fields in radiative zones (generated by the Tayler-Spruit dynamo). We find that all models fail to predict core rotation as slow as observed on the RGB and during core He burning, implying that an unmodeled angular momentum transport process must be operating on the early RGB of low mass stars. Later evolution of the star from the He burning clump to the cooling WD phase appears to be at nearly constant core angular momentum. We also incorporate the adiabatic pulsation code, ADIPLS, to explicitly highlight this shortfall when applied to a specific _Kepler_ asteroseismic target, KIC8366239.

"Like every great river and every great sea, the moon belongs to none and belongs to all. It still holds the key to madness, still controls the tides that lap on shores everywhere, still guards the lovers who kiss in every land under no banner but the sky". E.B. White The New Yorker, July 26, 1969Where does the Moon come from?Scientist believe that our Moon formed out of a ‘giant impact’ that occurred between a Mars-sized planet and the early Earth, some 4.5 billion years ago. The Moon was then formed from the coalescence of the orbiting debris scattered during the impact.Recent results seem to confirm this scenario

These instructions give you guidelines for preparing papers for IEEE TRANSACTIONS and JOURNALS. Use this document as a template if you are using Microsoft Word 6.0 or later. Otherwise, use this document as an instruction set. The electronic file of your paper will be formatted further at IEEE. Define all symbols used in the abstract. Do not cite references in the abstract. Do not delete the blank line immediately above the abstract; it sets the footnote at the bottom of this column.

Recent asteroseismic analyses have revealed the presence of strong (B≳10⁵ G) magnetic fields in the cores of many red giant stars. Here, we examine the implications of these results for the evolution of stellar magnetic fields, and we make predictions for future observations. Those stars with suppressed dipole modes indicative of strong core fields should exhibit moderate but detectable quadrupole mode suppression. The long magnetic diffusion times within stellar cores ensure that dynamo-generated fields are confined to mass coordinates within the main sequence convective core, and the sharp increase in dipole mode suppression rates above 1.5 M⊙ may be explained by the larger convective core masses and faster rotation of these more massive stars. In clump stars, core fields of $\sim 10^5 \, {\rm G}$ can suppress dipole modes, whose visibility should be equal to or less than the visibility of suppressed modes in ascending red giants. High dipole mode suppression rates in low-mass (M ≲ 2 M⊙) clump stars would indicate that magnetic fields generated during the main sequence can withstand subsequent convective phases and survive into the compact remnant phase. Finally, we discuss implications for observed magnetic fields in white dwarfs and neutron stars, as well as the effects of magnetic fields in various types of pulsating stars.