Podcasts about gw170817

fWotD Episode 2849: Virgo interferometer Welcome to Featured Wiki of the Day, your daily dose of knowledge from Wikipedia’s finest articles.The featured article for Friday, 21 February 2025 is Virgo interferometer.The Virgo interferometer is a large-scale scientific instrument near Pisa, Italy, for detecting gravitational waves. The detector is a Michelson interferometer, which can detect the minuscule length variations in its two 3-km (1.9 mi) arms induced by the passage of gravitational waves. The required precision is achieved using many systems to isolate it from the outside world, including keeping its mirrors and instrumentation in an ultra-high vacuum and suspending them using complex systems of pendula. Between its periodical observations, the detector is upgraded to increase its sensitivity. The observation runs are planned in collaboration with other similar detectors, including the two Laser Interferometer Gravitational-Wave Observatories (LIGO) in the United States and the Japanese Kamioka Gravitational Wave Detector (KAGRA), as cooperation between several detectors is crucial for detecting gravitational waves and pinpointing their origin.It was conceived and built when gravitational waves were only a prediction of general relativity. The project, named after the Virgo galaxy cluster, was first approved in 1992 and construction was completed in 2003. After several years of improvements without detection, it was shut down in 2011 for the "Advanced Virgo" upgrades. In 2015, the first observation of gravitational waves was made by the two LIGO detectors, while Virgo was still being upgraded. It resumed observations in early August 2017, making its first detection on 14 August (together with the LIGO detectors); this was quickly followed by the detection of the GW170817 gravitational wave, the only one also observed with classical methods (optical, gamma-ray, X-ray and radio telescopes) as of 2024.Virgo is hosted by the European Gravitational Observatory (EGO), a consortium founded by the French Centre National de la Recherche Scientifique (CNRS) and the Italian Istituto Nazionale di Fisica Nucleare (INFN). The broader Virgo Collaboration, gathering 940 members in 20 countries, operates the detector, and defines the strategy and policy for its use and upgrades. The LIGO and Virgo collaborations have shared their data since 2007, and with KAGRA since 2019, forming the LIGO-Virgo-KAGRA (LVK) collaboration.This recording reflects the Wikipedia text as of 00:51 UTC on Friday, 21 February 2025.For the full current version of the article, see Virgo interferometer on Wikipedia.This podcast uses content from Wikipedia under the Creative Commons Attribution-ShareAlike License.Visit our archives at wikioftheday.com and subscribe to stay updated on new episodes.Follow us on Mastodon at @wikioftheday@masto.ai.Also check out Curmudgeon's Corner, a current events podcast.Until next time, I'm long-form Ruth.

For your special NORDVPN discount and risk free 30 Day Money back guarantee, visit www.nordvpn.com/stuartgary and use the code STUARTGARY at checkout. Get your online privacy under control with the best in the business.The Space, Astronomy & Science Podcast.SpaceTime Series 27 Episode 33*The Black Hole that Ripped Apart a StarIn a cosmic display of destruction, astronomers have witnessed the closest recorded incident of a star being devoured by a supermassive black hole. The event, spotted in galaxy NGC 3799, was observed in visible light, offering unprecedented insights into these violent phenomena. The tidal disruption event, now cataloged as Assassin 23 BD, emitted less energy and faded more rapidly than typical cases, placing it in a unique classification and suggesting such occurrences may be more common than once thought.*Hunting New Physics in Neutron Star WrecksThe cataclysmic mergers of neutron stars could be hiding secrets of new physics, with potential clues about the enigmatic dark matter. The historic GW170817 collision, which sent ripples through space-time, has now been used to constrain theories on axion-like particles. These elusive entities could be part of the dark matter puzzle, and their traces might be detectable in future neutron star mergers, offering a new window into the fundamental workings of the universe.*Guardian Gas Giants and Their Terrestrial ChargesA new study suggests that Earth-like planets often come with Jupiter-like protectors. Simulations of planetary systems show that "dry" super-Earths and distant "cold" Jupiters frequently coexist, with the gas giants acting as cosmic shields. This relationship hints at a formation pattern where massive protoplanetary disks give rise to both rocky worlds and their gaseous sentinels, providing a glimpse into the architecture of alien solar systems.*China's Moonwalk Ambitions by 2030China has set its sights on the Moon, with plans to land taikonauts on the lunar surface before the end of the decade. The ambitious project involves the development of the Long March 10 rocket, a new spacecraft, and a lunar lander. In a two-launch scenario, the vehicles will rendezvous in lunar orbit, setting the stage for China's historic manned moon landing and furthering their collaboration with Russia on a lunar base.Plus, we examine the latest space news, delve into the science of extreme heat and preterm births, and explore the mystery of microplastics in human arteries.For more SpaceTime and to support the show, visit our website at https://spacetimewithstuartgary.com where you can access our universal listen link, find show notes, and learn how to become a patron.Listen to SpaceTime on your favorite podcast app with our universal listen link: https://spacetimewithstuartgary.com/listen and access show links via https://linktr.ee/biteszHQSupport the show: https://www.spreaker.com/podcast/spacetime-with-stuart-gary--2458531/supportFor more space and astronomy podcasts, visit our HQ at https://bitesz.com

Den 17. august 2017 blev en voldsom kollision mellem to neutronstjerner observeret.  Albert Sneppen har i en alder af blot 24 år sat sit betydelige aftryk i astrofysikkens verden med sin forskning i blandt andet sorte huller, galaksers udvikling og senest kolliderende neutronstjerner.  Han står bag et nyt studie af den kosmiske kollision med det mundrette navn GW170817. Studiet er for nyligt blevet udgivet i Nature, der er et af verdens førende tidsskrifter. Her fremsætter Sneppen og et hold af astrofysikere en banebrydende beskrivelse af, hvordan der i hjertet af den såkaldte kilonova foregår så ekstreme processer, at de muligvis kan skubbe til vores nuværende forståelse af fysikkens grundlag og universets udvidelseshastighed.  Kilonovaen er karakteriseret ved at forme en ildkugle, der er lige så fascinerende af astrofysiske årsager som af æstetiske. Eksplosionens sfæriske geometri er anderledes end for eksempel supernovaens – som er formet mere som en pandekage end her som en fodbold – og det er netop denne geometriske symmetri, der er ny for astrofysikerne og har trukket de store overskrifter.   Selv kalder Sneppen begivenheden for den perfekte eksplosion.   ** Albert Sneppen er ph.d.-studerende ved Niels Bohr Institutets Cosmic Dawn Center, hvor han forsker i sorte huller, udviklingen af galakser og kolliderende neutronstjerner.

GRB 230307A appartient à la classe des sursauts gamma de longue durée associés aux fusions d'objets compacts. Il a produit une kilonova similaire à AT2017gfo, associée à la fusion d'étoiles à neutrons détectée par les ondes gravitationnelles GW170817. Des astrophysiciens ont observé le signal rémanent de ce sursaut gamma avec le télescope Webb en infra-rouge, et ils ont découvert la présence d'éléments lourds comme du tellure... L'étude est publiée dans Nature.https://www.ca-se-passe-la-haut.fr/2023/10/du-tellure-detecte-par-la-telescope.html Source Heavy element production in a compact object merger observed by JWSTAndrew Levan et al.Nature (25 october 2023)https://doi.org/10.1038/s41586-023-06759-1 Illustrations Lumière rémanente de GRB 230307A imagées par le télescope Webb (NASA Webb Telescope Team) Spectre de la lumière rémanente de GRB 230307A obtenu avec le télescope Webb (NASA, ESA, CSA, Joseph Olmsted (STScI) Andrew Levan

Non-thermal emission from mildly relativistic dynamical ejecta of neutron star mergers by Gilad Sadeh et al. on Tuesday 29 November Binary neutron star mergers are expected to produce fast dynamical ejecta, with mildly relativistic velocities extending to $beta=v/c>0.6$. We consider the radio to X-ray synchrotron emission produced by collisionless shocks driven by such fast ejecta into the interstellar medium. Analytic expressions are given for spherical ejecta with broken power-law mass (or energy) distributions, $M(>gammabeta)propto(gammabeta)^{-s}$ with $s=s_{rm KN}$ at $gammabetagamma_0beta_0$ (where $gamma$ is the Lorentz factor). For parameter values characteristic of merger calculation results -- a "shallow" mass distribution, $1

Non-thermal emission from mildly relativistic dynamical ejecta of neutron star mergers by Gilad Sadeh et al. on Monday 28 November Binary neutron star mergers are expected to produce fast dynamical ejecta, with mildly relativistic velocities extending to $beta=v/c>0.6$. We consider the radio to X-ray synchrotron emission produced by collisionless shocks driven by such fast ejecta into the interstellar medium. Analytic expressions are given for spherical ejecta with broken power-law mass (or energy) distributions, $M(>gammabeta)propto(gammabeta)^{-s}$ with $s=s_{rm KN}$ at $gammabetagamma_0beta_0$ (where $gamma$ is the Lorentz factor). For parameter values characteristic of merger calculation results -- a "shallow" mass distribution, $1

Exploring the Phase Diagram of V-QCD with Neutron Star Merger Simulations by Tuna Demircik et al. on Monday 21 November Determining the phase structure of Quantum Chromodynamics (QCD) and its Equation of State (EOS) at densities and temperatures realized inside neutron stars and their mergers is a long-standing open problem. The holographic V-QCD framework provides a model for the EOS of dense and hot QCD, which describes the deconfinement phase transition between a dense baryonic and a quark matter phase. We use this model in fully general relativistic hydrodynamic (GRHD) simulations to study the formation of quark matter and the emitted gravitational wave signal of binary systems that are similar to the first ever observed neutron star merger event GW170817. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.10118v1

Impact of updated Multipole Love and f-Love Universal Relations in context of Binary Neutron Stars by Bikram Keshari Pradhan et al. on Tuesday 18 October Neutron star (NS) equation of state (EoS) insensitive relations or universal relations (UR) involving neutron star bulk properties play a crucial role in gravitational-wave astronomy. Considering a wide range of equations of state originating from (i) phenomenological relativistic mean field models, (ii) realistic EoS models based on different physical motivations, and (iii) polytropic EoSs described by spectral decomposition method, we update the EoS-insensitive relations involving NS tidal deformability (Multipole Love relation) and the UR between f-mode frequency and tidal deformability (f-Love relation). We analyze the binary neutron star (BNS) event GW170817 using the frequency domain TaylorF2 waveform model with updated universal relations and find that the additional contribution of the octupolar electric tidal parameter and quadrupolar magnetic tidal parameter or the change of multipole Love relation has no significant impact on the inferred NS properties. However, adding the f-mode dynamical phase lowers the 90% upper bound on $tilde{Lambda}$ by 16-20% as well as lowers the upper bound of NSs radii by $sim$500m. The combined URs (multipole Love and f-Love) developed in this work predict a higher median (also a higher 90% upper bound) for $tilde{Lambda}$ by 6% and also predict higher radii for the binary components of GW170817 by 200-300m compared to the URs used previously in the literature. We further perform injection and recovery studies on simulated events with different EoSs in $rm A+$ detector configuration as well as with third generation (3G) Einstein telescope. In agreement with the literature, we find that neglecting f-mode dynamical tides can significantly bias the inferred NS properties, especially for low mass NSs. However, we also find that the impact of the URs is within statistical errors. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.09425v1

Heavy elements and electromagnetic transients from neutron star mergers by S. Rosswog et al. on Sunday 16 October Compact binary mergers involving neutron stars can eject a fraction of their mass to space. Being extremely neutron rich, this material undergoes rapid neutron capture nucleosynthesis, and the resulting radioactivity powers fast, short-lived electromagnetic transients known as kilonova or macronova. Such transients are exciting probes of the most extreme physical conditions and their observation signals the enrichment of the Universe with heavy elements. Here we review our current understanding of the mass ejection mechanisms, the properties of the ejecta and the resulting radioactive transients. The first well-observed event in the aftermath of GW170817 delivered a wealth of insights, but much of today's picture of such events is still based on a patchwork of theoretical studies. Apart from summarizing the current understanding, we also point out questions where no consensus has been reached yet, and we sketch possible directions for the future research. In an appendix, we describe a publicly available heating rate library based on the WinNet nuclear reaction network, and we provide a simple fit formula to alleviate the implementation in hydrodynamic simulations. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2208.14026v2

Optical measurement of superluminal motion in the neutron-star merger GW170817 by Kunal P. Mooley et al. on Thursday 13 October The afterglow of the binary neutron star merger GW170817 gave evidence for a structured relativistic jet and a link between such mergers and short gamma-ray bursts. Superluminal motion, found using radio very long baseline interferometry (VLBI), together with the afterglow light curve provided constraints on the viewing angle (14-28 degrees), the opening angle of the jet core (less than about 5 degrees), and a modest limit on the initial Lorentz factor of the jet core (more than 4). Here we report on another superluminal motion measurement, at seven times the speed of light, leveraging Hubble Space Telescope precision astrometry and previous radio VLBI data of GW170817. We thereby obtain a unique measurement of the Lorentz factor of the wing of the structured jet, as well as substantially improved constraints on the viewing angle (19-25 degrees) and the initial Lorentz factor of the jet core (more than 40). arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.06568v1

GW170817 4 5 years after merger: Dynamical ejecta afterglow constraints by Arvind Balasubramanian et al. on Wednesday 12 October GW170817 is the first binary neutron star (NS) merger detected in gravitational waves (GWs) and photons, and so far remains the only GW event of its class with a definitive electromagnetic (EM) counterpart. Radio emission from the structured jet associated with GW170817 has faded below the sensitivity achievable via deep radio observations with the most sensitive radio arrays currently in operation. Hence, we now have the opportunity to probe the radio re-brightening that some models predict, should emerge at late times from the interaction of the dynamically-stripped merger ejecta with the interstellar medium. Here we present the latest results from our deep radio observations of the GW170817 field with the Karl G. Jansky Very Large Array (VLA), 4.5 years after the merger. Our new data at $3,$GHz do not show any compelling evidence for emission in excess to the tail of the jet afterglow ($

Reconstructing the neutron star equation of state from observational data via automatic differentiation by Shriya Soma et al. on Monday 19 September The equation of state (EoS) that describes extremely dense matter under strong interactions is not completely understood. One reason is that the first-principle calculations of the EoS at finite chemical potential are challenging in nuclear physics. However, neutron star observables like masses, radii, moment of inertia and tidal deformability are direct probes to the EoS and hence make the EoS reconstruction task feasible. In this work, we present results from a novel deep learning technique that optimizes a parameterized equation of state in the automatic differentiation framework. We predict stellar structures from a pre-trained Tolman-Oppenheimer-Volkoff (TOV) solver network, given an EoS represented by neural networks. The latest observational data of neutron stars, specifically their masses and radii, are used to implement the chi-square fitting. We optimize the parameters of the neural network EoS by minimizing the error between observations and predictions. The well-trained neural network EoS gives an estimate of the relationship between the pressure and the mass density. The results presented are consistent with those from conventional approaches and the experimental bound on the tidal deformability inferred from the gravitational wave event, GW170817. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.08883v1

Spectroscopic r-Process Abundance Retrieval for Kilonovae I: The Inferred Abundance Pattern of Early Emission from GW170817 by Nicholas Vieira et al. on Thursday 15 September Freshly-synthesized r-process elements in kilonovae ejecta imprint absorption features on optical spectra, as observed in the GW170817 binary neutron star merger. These spectral features encode insights into the physical conditions of the r-process and the origins of the ejected material, but associating features with particular elements and inferring the resultant abundance pattern is computationally challenging. We introduce Spectroscopic r-Process Abundance Retrieval for Kilonovae (SPARK), a modular framework to perform Bayesian inference on kilonova spectra with the goals of inferring elemental abundance patterns and identifying absorption features at early times. SPARK inputs an atomic line list and abundance patterns from reaction network calculations into the TARDIS radiative transfer code. It then performs fast Bayesian inference on observed kilonova spectra by training a Gaussian process surrogate for the approximate posteriors of kilonova ejecta parameters, via active learning. We use the spectrum of GW170817 at 1.4 days to perform the first inference on a kilonova spectrum, and recover a complete abundance pattern. Our inference shows that this ejecta was generated by an r-process with either (1) high electron fraction Y_e ~ 0.35 and high entropy s/k_B ~ 25, or, (2) a more moderate Y_e ~ 0.30 and s/k_B ~ 14. These parameters are consistent with a shocked, polar dynamical component, and a viscously-driven outflow from a remnant accretion disk, respectively. We also recover previous identifications of strontium absorption at ~8000 AA, and tentatively identify yttrium and/or zirconium at < 4500 AA. Our approach will enable computationally-tractable inference on the spectra of future kilonovae discovered through multi-messenger observations. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.06951v1

3D radiative transfer kilonova modelling for binary neutron star merger simulations by Christine E. Collins et al. on Monday 12 September The detection of GW170817 and the accompanying electromagnetic counterpart, AT2017gfo, have provided an important set of observational constraints for theoretical models of neutron star mergers, nucleosynthesis, and radiative transfer for kilonovae. We apply the 3D Monte Carlo radiative transfer code ARTIS to produce synthetic light curves of the dynamical ejecta from a neutron star merger, which has been modelled with 3D smooth-particle hydrodynamics (SPH) and included neutrino interactions. Nucleosynthesis calculations provide the energy released from radioactive decays of r-process nuclei, and radiation transport is performed using grey opacities given as functions of the electron fraction. We present line-of-sight dependent bolometric light curves, and find the emission along polar lines of sight to be up to a factor of ~2 brighter than along equatorial lines of sight. Instead of a distinct emission peak, our bolometric light curve exhibits a monotonic decline, characterised by a shoulder at the time when the bulk ejecta becomes optically thin. We show approximate band light curves based on radiation temperatures and compare these to the observations of AT2017gfo. We find that the rapidly declining temperatures lead to a blue to red colour evolution similar to that shown by AT2017gfo. We also investigate the impact of an additional, spherically symmetric secular ejecta component, and we find that the early light curve remains nearly unaffected, while after about 1 day the emission is strongly enhanced and dominated by the secular ejecta, leading to the shift of the shoulder from 1-2 to 6-10 days. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.05246v1

The Astronomy, Technology, and Space Science News Podcast.SpaceTime Series 25 Episode 28*How Russia's war against Ukraine has changed space operationsNASA and the European Space Agency are exploring new ways to keep the International Space Station flying without the Russian Federal Space Agency Roscosmos -- as tensions continue to worsen following Russia's invasion of Ukraine. Moscow has undertaken a full-scale attack against Ukraine leaving thousands dead and over a million refugees fleeing the war zone.*Discovery of a kilonovaAstronomers may have detected a “sonic boom” from a powerful blast known as a kilonova. This event was seen in GW170817, a merger of two neutron stars and the first object detected in both gravitational waves and electromagnetic radiation, or light.*Rocket Lab's new second launch pad opens for businessRocket Lab have successfully launched their first mission from the company's new launch pad B at their Mahia Peninsula launch complex on New Zealand's North Island east coast. Construction of the second launch pad at the complex began in December 2019.*The Science ReportStudy shows significant changes in the brains of people who have suffered COVID-19.Research shows air pollution is shortening people's lives by nearly three years.The last meal of a 95 million year old crocodile unearthed in Queensland was a dinosaur.How dogs and people are more similar than you think.Skeptic's guide to poltergeist investigationsListen to SpaceTime on your favorite podcast app with our universal listen link: https://link.chtbl.com/spacetime For more SpaceTime and show links: https://linktr.ee/biteszHQ If you love this podcast, please get someone else to listen to. Thank you…To become a SpaceTime supporter and unlock commercial-free editions of the show, gain early access and bonus content, please visit https://bitesz.supercast.com/ . Premium version now available via Spotify and Apple Podcasts.For more podcasts visit our HQ at https://bitesz.com

L'événement GW170817 qui a vu le 17 août 2017 la fusion de deux étoiles à neutrons dans une myriade de rayonnements à toutes les longueurs d'ondes, des ondes radio aux ondes gravitationnelles en passant par les infra-rouges, les rayons X et les rayons gamma a très probablement produit un trou noir, qui serait le plus petit que l'on connaisse. Mais ce trou noir est-il né tout de suite après la fusion des étoiles à neutrons ? Une observation du signal de rayons X résiduel de la collision apporte une réponse. L'étude est à paraître dans The Astrophysical Journal Letters.

L'événement gravitationnel GW170817 correspondant à la fusion de deux étoiles à neutrons avec la détection simultanée d'une contrepartie électromagnétique dans toutes les longueurs d'ondes avaient permis aux astrophysiciens de déterminer q'un tel événement pouvait être à l'origine de la production d'éléments lourds, comme l'or en particulier. Mais une nouvelle étude venant de paraître calcule exactement toutes les sources astrophysiques des éléments chimiques, et l'or reste un cas à part : il n'y a pas assez de fusions d'étoiles à neutrons pour fabriquer tout l'or des galaxies... Une étude acceptée pour publication dans The Astrophysical Journal.

Lorsque deux étoiles à neutrons entrent en collision, des rayonnements dans à peu près toutes les longueurs d'ondes sont produits, en plus des ondes gravitationnelles liées à la coalescence. C'est ce qu'avait très bien montré l'événement GW170817 il y a trois ans. Aujourd'hui, une équipe d'astrophysiciens montrent que des signes avant coureurs d'une telle fusion/collision pourraient être détectés avant l'apparition des ondes gravitationnelles, sous le forme d'ondes radio très particulières. Une étude parue dans The Astrophysical Journal Letters.

Почему теории струн нужны 11 измерений, что не так с гравитацией, как бороться с затоплением космических кораблей, почему перегреваются электомобили и боятся ли вампиры лунного света — все это в новом выпуске Теории Большой Бороды. Ведущий: Антон Поздняков Темы [00:00:33] ⋅⋅⋅ Приветствие [00:01:49] ⋅⋅⋅ Для чего нужны дополнительные пространственные измерения в физике The Big Beard Theory 105 — Что такое теория струн [00:03:19] ⋅⋅⋅ Чем гравитация отличается от остальных трех фундаментальных взаимодействий [00:08:03] ⋅⋅⋅ Мысленный эксперимент — как понять дополнительные пространствапространственные изменерия и эффекты, которые они дают для гравитации [00:11:37] ⋅⋅⋅ Как гравитационные волны могут помочь узнать о дополнительных измерениях Что такое гравитационные волны The Big Beard Theory 130 — Килонова [00:15:23] ⋅⋅⋅ Статья «Предельное количество пространовенно-временных измерений на основе GW170817» [00:23:13] ⋅⋅⋅ Ответы на вопросы слушателей [00:24:07] ⋅⋅⋅ Как на МКС решают проблему с воздухом [00:25:12] ⋅⋅⋅ Что правильнее, Теория Относительности или Квантовая Механика [00:27:53] ⋅⋅⋅ Почему вампиры не боятся отраженного от Луны солнечного света [00:30:58] ⋅⋅⋅ Почему электродвигатели перегреваются на больших скоростях [00:34:30] ⋅⋅⋅ Как бороться с затоплением космических кораблей [00:35:29] ⋅⋅⋅ Почему для защиты от радиации при межпланетных перелетах не генерировать собственное магнитное поле [00:37:00] ⋅⋅⋅ Планы сбора космических кораблей не на Земле, а на орбите [00:38:04] ⋅⋅⋅ Прощание Поддержи Бородокаст Patreon Подписывайся Наши подкасты: BeardyBuilding | BeardyCast | The Big Beard Theory Свои вопросы присылайте на почту ap@beardycast.com. Вступай в наш публичный чат и читай наш новостной канал в Телеграме. Не знаете как подписаться на подкаст? Читайте статью «Как слушать подкасты»!

La fusion de deux étoiles à neutrons le 17 août 2017 a été une occasion incroyable pour les astrophysiciens pour comprendre de nombreux phénomènes, à commencer par les phénomènes qu'on appelle les kilonovas et les GRB courts ou encore la naissance d'un trou noir signant sa présence par un jet de matière et de rayonnement. Mais cette collision de deux étoiles à neutrons a aussi été une occasion en or pour mieux comprendre les étoiles à neutrons elles-mêmes.

Une association de trois réseaux de radiotélescopes parmi les plus performants du monde a permis de déterminer la vitesse du jet relativiste émanent du résidu de la fusion de deux étoiles à neutrons observée en 2017 et répertorié GW170817. La vitesse apparente atteint 4 fois la vitesse de la lumière, une illusion supraluminique due à la vitesse ultra-relativiste du jet qui se trouve légèrement désaxé par rapport à la ligne de visée.

La fusion des deux étoiles à neutrons à l'origine de l'événement gravitationnel GW170817 de l'été dernier a très probablement produit un trou noir. Cette conclusion est le résultat de l'analyse de données en rayons X obtenues avec le télescope spatial Chandra dans les mois qui ont suivi l'événement cataclysmique.

A new study using Chandra data of GW170817 indicates that the event that produced gravitational waves likely created the lowest mass black hole known.

In this podcast, we first share report  of a new brightening of a YSO – that’s a “Young Stellar Object” – known as EC 53 in Serpens Main, in ATel 11614.  A YSO is a star which is still in the process of formation, undergoing gravitational collapse, just as nuclear burning is attempting to get … Continue reading OTN Ep #010: Young Stellar Object EC 53, and Gravitational Wave Source GW170817 →

L'observation de la fusion d'étoiles à neutrons du 17 août 2017 qui a donné lieu à l'événement d'ondes gravitationnelles GW170817 et à la bouffée de rayons gamma GRB 170817A a aussi émis quantités d'ondes radio et de rayons X. Il y a quelques semaines, je vous relatais l'observation d'une augmentation de l'intensité de la rémanence en ondes radio. Aujourd'hui, c'est au tour des rayons X de montrer une augmentation, 109 jours après le cataclysme...

L'observation astrophysique la plus marquante de l'année 2017, la fusion de deux étoiles à neutrons observées à 130 millions d'années-lumière en multi-longueurs d'ondes et multi-messagers (ondes gravitationnelles et photons) a permis de répondre à de nombreuses questions. Mais le suivi de l'émission radio du résidu de la collision depuis ce fameux 17 août 2017 indique une augmentation du signal au lieu d'une décroissance, une anomalie qui permet d'en savoir encore plus sur ce qui s'est passé et se passe encore.

La tertulia semanal en la que repasamos las últimas noticias de la actualidad científica. En el episodio de hoy: Energía oscura y constante cosmológica; Implicaciones de la detección multimensajero de ondas gravitacionales GW170817 sobre la cosmología; El futuro magnético del Sol; Detectado un asteroide que podría provenir de fuera del Sistema Solar; Entrevista Dr. Francisco-Shu Kitaura. En la foto, de arriba a abajo y de izquierda a derecha: Javier Licandro, Jose Alberto Rubiño, Héctor Vives, Héctor Socas. Todos los comentarios vertidos durante la tertulia representan únicamente la opinión de quien los hace… y a veces ni eso. CB:SyR es una colaboración entre el Área de Investigación y la Unidad de Comunicación y Cultura Científica (UC3) del Instituto de Astrofísica de Canarias.

La tertulia semanal en la que repasamos las últimas noticias de la actualidad científica. En el episodio de hoy: Energía oscura y constante cosmológica; Implicaciones de la detección multimensajero de ondas gravitacionales GW170817 sobre la cosmología; El futuro magnético del Sol; Detectado un asteroide que podría provenir de fuera del Sistema Solar; Entrevista Dr. Francisco-Shu Kitaura. En la foto, de arriba a abajo y de izquierda a derecha: Javier Licandro, Jose Alberto Rubiño, Héctor Vives, Héctor Socas. Todos los comentarios vertidos durante la tertulia representan únicamente la opinión de quien los hace… y a veces ni eso. CB:SyR es una colaboración entre el Área de Investigación y la Unidad de Comunicación y Cultura Científica (UC3) del Instituto de Astrofísica de Canarias.

Laidoje Ronaldas Macas Ligo konsorciumo narys apie dviejų neutroninių žvaigždžių susidūrimą, užfiksuotą gravitacinėmis bangomis, - GW170817. Vedėjas Bernardas šaknys.

Laidoje Ronaldas Macas Ligo konsorciumo narys apie dviejų neutroninių žvaigždžių susidūrimą, užfiksuotą gravitacinėmis bangomis, - GW170817. Vedėjas Bernardas šaknys.

Laidoje Ronaldas Macas Ligo konsorciumo narys apie dviejų neutroninių žvaigždžių susidūrimą, užfiksuotą gravitacinėmis bangomis, - GW170817. Vedėjas Bernardas šaknys.

Laidoje Ronaldas Macas Ligo konsorciumo narys apie dviejų neutroninių žvaigždžių susidūrimą, užfiksuotą gravitacinėmis bangomis, - GW170817. Vedėjas Bernardas šaknys.

Astronomers have used NASA's Chandra X-ray Observatory to make the first X-ray detection of a gravitational wave source.