INTRODUCTION Lorem ipsum dolor sit amet, consectetur adipiscing elit. Cras egestas auctor molestie. In hac habitasse platea dictumst. Duis turpis tellus, scelerisque sit amet lectus ut, ultricies cursus enim. Integer fringilla a elit at fringilla. Lorem ipsum dolor sit amet, consectetur adipiscing elit. Nulla congue consequat consectetur. Duis ac mi ultricies, mollis ipsum nec, porta est. Mauris nec massa leo. Mauris ac diam auctor nisl imperdiet porta. Sed sit amet neque eget nisi dictum placerat. Duis sit amet pellentesque odio. Cras scelerisque sem a consectetur vehicula. Aliquam interdum luctus fringilla. Nunc sollicitudin, lorem in semper viverra, dui nisi sodales sem, ut condimentum erat leo eget arcu. Donec pharetra aliquam metus, non pulvinar tellus interdum a. Mauris a ante pharetra, mollis enim in, eleifend erat. Pellentesque suscipit risus massa, non vestibulum libero euismod feugiat. In hac habitasse platea dictumst. Maecenas rutrum lobortis lobortis. Vestibulum convallis porttitor sem ac ultricies. Mauris volutpat fringilla nisl blandit semper. Proin nec iaculis sem. Aenean neque ipsum, pretium a faucibus non, tincidunt ut sapien. Nunc a aliquet sem, eget aliquet purus. Vestibulum ac placerat mauris. Proin sed dolor ac justo semper iaculis. Donec varius, nibh sit amet finibus tristique, sapien ante interdum odio, et pretium sapien libero nec massa. In hac habitasse platea dictumst. Donec vel augue ac sapien imperdiet pretium. Maecenas gravida risus id ultricies dignissim. Maecenas gravida felis quis dolor faucibus, sed maximus lorem tristique. Nam hendrerit quam quis ante porta posuere. Fusce finibus maximus orci at porttitor. Nulla tempor ex a porttitor consequat. Quisque quis tempor eros. Donec nisi mauris, sollicitudin in dapibus eu, interdum ultricies quam. Pellentesque tincidunt lobortis orci non venenatis. Cras in justo luctus, pulvinar augue id, suscipit diam. Morbi aliquet fringilla nibh, vel pellentesque dui venenatis eget. Orci varius natoque penatibus et magnis dis parturient montes, nascetur ridiculus mus. Donec ultricies ultrices magna gravida porta. Maecenas accumsan diam dui, auctor ornare ex pellentesque id. Integer tempus massa id augue finibus convallis. Nulla vestibulum, nisl id tempor pulvinar, felis dui pellentesque lacus, quis bibendum metus enim sed ex. Duis magna nunc, rutrum sodales elementum a, egestas eget dolor. Vivamus non pretium nunc, at vestibulum arcu. Vivamus pharetra, justo vel blandit feugiat, magna neque feugiat mi, a bibendum erat arcu a est. Sed vestibulum, leo non elementum condimentum, dui ipsum vehicula quam, a vehicula turpis ipsum a nibh. Mauris posuere lobortis porta. Aenean augue neque, varius vitae dapibus ac, dictum ut nisl.

A NEW COLLABORATIVE TOOL COULD REVOLUTIONIZE SCIENTIFIC AUTHORSHIP. Originally published by Scientific American

During the night of August 11th, a meteor shower called ’Perseids’ might put up a memorable show. After the moon sets, which occurs around 1:00 AM local time, it might be possible to see up to 200 ’shooting stars’ per hour. Below, what you need to know about this astronomical event. WHAT IS A SHOOTING STAR? Despite their name, shooting stars are actually small rocks (meteoroids) falling towards the Earth due to our planet’s gravitational attraction. As they move rapidly through the atmosphere, they reach very high temperatures due to friction with air particles. This makes them burn and become visible to the human eye. The trail they leave is called ’Meteor’. Due to their tiny size, they usually almost completely burn in a fraction of a second. In some very exceptional cases, large meteors can continue the hot descent and hit the ground. If they also survive the crash, they get promoted immediately to the ’meteorites’ class. Generally speaking a meteoroid producing a meteor needs to be at least as large as a marble to reach the Earth and eventually become a meteorite. Some Burning facts: - Average meteorite velocity: 30000 miles/hour (48000 km/h) - Max temperature: 3000 F (1650 C) - The Meteor Crater in Arizona was formed 50000 years ago by an object 160 feet (50 meters) across - ... yes, impacts like the one that produced the Meteor Crater are extremely rare

This is a layman summary of “Local Radiation Hydrodynamic Simulations of Massive Star Envelopes at The Iron Opacity Peak” from Yan-Fei Jiang (姜燕飞), Matteo Cantiello , Lars Bildsten, Eliot Quataert and Omer Blaes. The full article can be downloaded from the arXiv. This layman summary is part of the Public Friendly Open Science initiative.

CERN's 2008 Large Hadron Collider is not just the world's largest and most powerful particle collider but also the largest single machine and most complex experimental facility. Here, physicists are able to test fundamental physics theories by smashing particles with extremely high energies. On 8 October 2013 the Nobel prize in physics was awarded jointly to François Englert and Peter Higgs "for the theoretical discovery of a mechanism that contributes to our understanding of the origin of mass of subatomic particles, and which recently was confirmed through the discovery of the predicted fundamental particle, by the ATLAS and CMS experiments at CERN's Large Hadron Collider."

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Peer review is arguably necessary for effective communication amongst researchers.  Authors, editors, and the public rely on peer review to ensure a first measure of trust in scientific communication.  While peer review is considered to be integral in scholarly communication by most, its shortcomings are becoming evident. Former editor of JAMA and NEJM Drummond Rennie once said, "if peer review was a drug it would never be allowed onto the market." Is this true? Does peer review, as it is done today, cause more harm than good?

What does being a scientist mean to you?To me, science is about thinking rationally, solving problems and enjoying learning new things about the universe. People who are not professional scientists can also be scientists. This is the idea behind "citizen science" projects: https://www.zooniverse.org. You, too, can be a scientist, even if it’s only for an hour at a time!  Can you summarize the main focus of your research and what drew you to that field of study/work?I use numerical simulations to model how stars like our sun formed. When I was a physics graduate student I was interested in working on some kind of computational modeling. It turns out there are a lot of really interesting complex problems in astrophysics that you can only study with large computers. The study of star formation has a lot of different physics in it: gravity, magnetic fields, turbulence, and radiation. These interact in nonlinear and sometimes unexpected ways, which make star formation a fun thing to model. I also use the simulations to make cool movie

Thomas Edison has an impressive 2,332 worldwide patents. Some of his well-known inventions include the phonograph, motion pictures, and the magnetic iron ore separator. After the success of his first major invention, the quadruplex telegraph, Edison wanted to build his own laboratory so that he could continue to innovate. In 1875, he purchased around 34 acres in Raritan Township, NJ and built the "Invention Factory". By Spring 1876, the Invention Factory consisted of a main laboratory, ancillary buildings, a carpenters’ shop, carbon shed, and blacksmith shop. His first breakthrough at the Invention Factory, the phonograph, produced the first voice recording (“Mary Had a Little Lamb”) and earned Edison the title, “The Wizard of Menlo Park”.

The search for extrasolar planets (EXOPLANETS) is one of the most rapidly expanding fields in astrophysics. Thanks to recent space-based efforts the number of detected planets in extrasolar stellar systems has increased dramatically, and more than 900 objects have been identified as of today, see e.g. http://exoplanet.eu/catalog/. With candidates identified in the so-called habitable zone (HZ)[1] the question of extraterrestrial life becomes very actual. Here we discuss ideas that could lead to infer the presence (or the past existence) of an extraterrestrial civilization by the detection of artifacts in orbit around the host planet. [1] The theoretical band around a star where a planet could orbit and host liquid water

THEORY OF EVOLUTION AND DEATH OF MASSIVE STARS Overview of the material that will be covered at the “Look & Listen” School 2014 Abstract We will first cover some basic principles of stellar evolution, with a particular emphasis on the physics of massive stars. Then we will focus on the phenomena that are currently believed to prominently influence the life of massive stars and determine the conditions at the pre-SN stage. Informed by the most recent observational results, we will also focus on some unsolved problems in stellar physics and how they could impact the death of massive stars and their stellar remnants. Schedule 1. Tuesday 14 Jan - Principles of stellar evolution (20+10) - Massive Stars evolution: Main Sequence and He-Burning (20+10) - Massive Stars evolution: Late evolutionary stages (20+10) 2. Thursday 16 Jan - Stellar Rotation (20+10) - Stellar Rotation and Magnetic Fields (20+10) - Mass loss (20+10) 3. Friday 17 Jan - Massive Binary Stars (20+10) - Very Massive Stars (20+10) - Progenitors of NS/BH, SNe, PISNe, GRBs (20+10)

This collaborative document has been created for the panel discussion on “Rotation in massive stars” (FOE 2015). All conference participants have been added to the document and can edit / comment / add figures (just drag&drop) / references and even LaTeX equations if needed (check the help page for more infos on how to edit the document). Hopefully this will capture the essential ideas and interactions that will stem during and after the discussion. The document can be forked at any time, so that particular discussions can be taken further and potentially lead to active collaborations.

Our goal is to reconstruct pre-SN mass-loss history using radio variability observations and constrain the dominant mass-loss mechanism during the last few hundred years of massive star evolution. We will draw from existing observations to re-design the strategy for future observing campaigns.

A variety of research demonstrates that humans learn and communicate best when more than one processing system is used . Authorea - a leading collaboration platform to write, share and openly research in realtime - allows people to author manuscripts and include rich media, such as data sets, software, source code and videos. The media-rich, data-driven capabilities Authorea make it the perfect platform to create and disseminate a new generation of research articles, which are natively web-based, open, and reproducible.

The Hubble image of the Bubble Nebula (NGC 7635) is the official image celebrating the 26th anniversary of Hubble's launch into Earth orbit's. Since 1990 Hubble has been capturing awe-inspiring images of the Universe. Floating about 350 miles above the Earth, the Hubble Space Telescope (HST) is able to take high-resolution images free of the image-distortion that occurs due to atmospheric turbulence. Hubble performs a full orbit around the Earth approximately every 95 minutes, and since its launch has completed 1.2 million observations. Among its many accomplishments, HST helped scientists determine the rate of expansion of the Universe.

É stato dimostrato per la prima volta che é possibile determinare la presenza di intensi campi magnetici nelle regioni interne di stelle evolute. Questo puó essere fatto grazie all’asterosismologia, una disciplina simile alla sismologia ma applicata ai corpi celesti. L’asterosismologia sfrutta la presenza di onde che si propagano attraverso oggetti astronomici come le stelle, per determinarne le proprietá interne. Questo é analogo a un’ecografia, in cui si usano onde sonore per ottenere immagini di parti altrimenti invisibili del corpo umano. Le regioni esterne delle giganti rosse, stelle piú anziane del sole e con un raggio maggiore, sono caratterizzate da movimenti convettivi turbolenti che causano onde sonore. Questo é simile al rumore prodotto dall’acqua che bolle in una pentola. Queste onde si propagano all’interno della stella e a loro volta generano un altro tipo di onde (le onde di gravitá, da non confondersi con le onde gravitazionali). La forza responsabile per il moto oscillatorio delle onde di gravitá é la stessa responsabile per il galleggiamento dei corpi nell’acqua. Infatti le onde del mare sono un tipo particolare di onde di gravitá. In pratica quello che succede é che le onde sonore si propagano negli stati esterni della stella, che ’suona’ come un gigantesco strumento musicale. Nelle giganti rosse l’energia associata con queste onde sonore riesce a far oscillare anche gli strati piú profondi della stella, appunto sotto forma di onde di gravitá che si propagano fin nel nucleo stellare. Questa specie di interferenza tra i due tipi di onde richiede che un pó dell’energia presente nei moti oscillatori acustici che caratterizzano gli strati esterni, venga trasferita ai moti oscillatori che avvengono nel nucle della stella sotto forma di onde di gravitá. Se peró nel nucleo sono presenti dei campi magnetici, la situazione puó cambiare. Questo avviene se i campi magnetici sono abbastanza intensi da alterare la propagazione delle onde di gravitá. Il campo magnetico in questo caso puó essere immaginato come un grosso elastico che intrappola il gas stellare. Un’onda di gravitá, come un’onda del mare, prova a creare uno spostamento del fluido (in questo caso il gas) a cui peró si oppone la tensione dell’elastico. In questa situazione la propagazione delle onde viene alterata fino a indurre una specie di intrappolamento. Questo effetto é stato battezzato “Effetto serra magnetico”. Quando le onde di gravitá sono intrappolate dal campo magnetico, l’energia che avevano ottenuto a scapito delle oscillazioni acustiche degli strati esterni viene formalmente persa. Qusto si ripercuote in una diminuzione dell’ampiezza delle oscillazioni visibile alla superficie della stella. Questa diminuzione dell’ampiezza delle oscillazioni é stata in effetti osservata dal telescopio spaziale Kepler in un gruppo di giganti rosse. Kepler é in grado di misurare variazioni piccolissime della luminositá di una stella (una parte in un milione). Perció é possibile porre dei limiti o addirittura misurare il campo magnetico interno per alcune di queste stelle. Il risultato é sensazionale: Alcune di queste stelle posseggono campi magnetici intensissimi nei loro nuclei, milioni di volte piú intensi del campo associato a un tipico magnete da frigorifero. Questo rappresenta un importantissimo passo avanti nella comprensione delle stelle, poiché questi campi magnetici hanno un ruolo fondamentale per l’evoluzione stellare e le proprietá degli stadi finali della vita di una stella. Per esempio alcune delle esplosioni piú luminose nell’universo (i lampi di raggi gamma) potrebbero essere associate con la morte di stelle con massa 10 o piú volte maggiore del sole, che hanno mantenuto un forte campo magnetico nel loro nucleo.

Dear Dr. Berlinsky, Please consider our application for a 1 week visit following the KITP program “Galactic Archaeology and Precision Stellar Astrophysics”. The proposing team wants to meet again to continue some very exciting work that was started at KITP and led to groundbreaking results in the field of stellar physics and asteroseismology. Please find below a brief description of the results that the team achieved during/after the KITP program and the follow up work we intend to perform while together at KITP. A team justification closes this application. We would like to meet at KITP either on 15-22 NOVEMBER (strong preference for this week) or 6-13 December. INTRODUCTION The team members enjoyed a very productive period of collaboration during the Galactic Archaeology and Precision Stellar Astrophysics program at KITP in 2015. That collaboration led to two papers on red giant asteroseismology, recently submitted to Science and Nature. The first paper discussed the ability to measure internal magnetic fields in red giant stars using asteroseismology, and the second used this technique to constrain/measure magnetic fields in the core of thousands of red giant stars. We believe this work has paved the way to a new sub-field of stellar astrophysics that is ripe for additional study. Consequently, there are several research topics which we wish to pursue during a follow-up visit to KITP. PROJECT OVERVIEW The first research topic we intend to investigate is the EXISTENCE OF STRONG MAGNETIC FIELDS WITHIN STARS ON THE RED CLUMP. The previous works only analyzed stars ascending the red giant branch, but similar physics will occur for red clump stars burning helium in their cores. However, identifying the asteroseismic signature of strong magnetic fields in clump stars is slightly more difficult because they are difficult to distinguish from ascending red giants. Collaboration between the team members will allow us to work out the details of this process from the observational end, and what can be learned from these observations on the theoretical end. A second topic of investigation are “DROOPY-LIKE” STARS that show a particular asteroseismic signature that allows for a more precise measurement of their internal magnetic fields. Thus far, only one star KIC 8561221 (“Droopy”) that shows this signature has been analyzed in detail (Garcia et al. 2014). However, more Droopy-like stars likely exist. We intend to identify these stars in the data, measure their internal magnetic field strengths, and use them to trace the evolution of internal magnetic field strengths in red giant stars. Third, we hope to use additional time at KITP to examine the OCCURRENCE OF MAGNETIC FIELDS IN CLUSTER STARS. These stars have nearly identical ages and compositions and provide the perfect testbed to understand evolution of magnetic fields in a uniform population of stars. Red giant cluster stars exist in both Kepler data and recent and upcoming K2 fields, with substantial data already secured by the team. These red giants are found in several clusters (of differing ages and metallicities) and can be used to understand the development of magnetic fields in different populations of stars. As a fourth research topic (time permitting) we will try to CONSTRAIN THE GEOMETRY OF INTERNAL MAGNETIC FIELDS in red giants with suppressed dipoles, using the scattering properties of dipolar gravity waves on the magnetic fields. Proposing Team and Team Justification 1. Lars Bildsten (KITP resident) 2. Matteo Cantiello (KITP resident) 3. Jim Fuller (Caltech) 4. Rafael A. Garcia (CEA, Paris) 5. Stéphane Mathis (CEA, Paris) 6. Dennis Stello (Sydney University) Five of the six team members outlined above are the main authors in the two papers submitted to Science (Theory) and Nature (Observations). Thanks to their complementary expertises, this group of scientists found a remarkable synergy while at KITP. Thanks to the presence of both theorists and observers, we were able to quickly identify an observational puzzle, find a theoretical explanation and test it on brand new data. In the process this led to the discovery of a novel, powerful way to look for magnetic fields in stellar interiors. The team has remained in touch and active after meeting at KITP, but it’s clear that only re-creating a full-immersion atmosphere can lead to rapid progress on the follow-up research program.

Despite its importance for the evolution and final end states of stars, the physics of stellar angular momentum transport remains poorly understood. Recent advances in ensemble asteroseismology has yielded measurements of core rotation in many ascending red giant branch stars (RGB) . The main result (Fig [period]) is that the cores of these stars are rotating at least 10 times slower than what is predicted by state-of-the art models . Moreover, detailed asteroseismic modeling shows that the bulk of radial differential rotation is localized in the radiative region between the H-burning shell and the bottom of the convective envelope . The magnetorotational instability (MRI) has been extensively studied in the context of angular momentum transport in accretion disks. However, it is not clear what role–if any–it might play in the radiative regions of differentially rotating stars. The existing literature is limited , and attempts to simulate this mechanism in stellar interiors have not yielded complete results appropriate for inclusion in stellar evolution codes. We propose to investigate the role of the MRI in stars using simulations that account for the important physical ingredients of stellar radiative regions: stable radial stratification, mean molecular weight gradients, differential rotation, and magnetic fields. These effects are parameterized by the Brunt-Väisälä frequency N, background gradient ∇μ, shear parameter q = dlogΩ/dlogR, and plasma β. emphasized the importance _double-diffusive_ effects in the stellar MRI. These effects occur when there is an imbalance between the microphysical dissipation of momentum ν, magnetic field η, and heat χ. In their analysis, they note that double diffusive effects can both stabilize and destabilize depending on the relative ratio of these coefficients. Here, we will carefully consider the effects of double-diffusive effects by a series of fast, linear solutions to characterize the parameter space most relevant to stellar parameters. Using the Dedalus framework, we will simulate the MRI in a simplified geometry to extract effective torques over a range of parameters. We will then implement these results in a 1D implementation in the MESA code to test against the full set of observations available: the core rotation of red giants, the solar core rotation profile, and the final spin rate of compact remnants. This project is extremely ambitious owing to the many length scales that must be resolved simultaneously and the very large parameter space to be spanned. However, we have at our disposal the ideal tools to make significant progress: the spectral magnetohydrodynamic simulation framework Dedalus and the extremely flexible stellar evolution code MESA. Dedalus provides an excellent platform to study the MRI in stellar interiors: it can be adapted to include the new terms and its spectral accuracy ensures that the widest possible dynamic range for a given resolution (Fig. [Dedalus]). Thanks to the extraordinary results from Kepler asteroseismology and the versatility of the open stellar evolution code MESA, we will be able to immediately test our results against the observations. This project could lead to a novel theory for internal angular momentum transport in stellar interiors, and, among other results, to updated predictions for SN and GRB progenitors. Both the Dedalus and MESA codes are fully open, so our results will be fully testable and reproducible by the astrophysics community. We will publish not only our results, but also our input files and configuration for both codes.