Podcasts about asteroseismology

Polaris Dawn launches and completes the first private spacewalk, the surface of a giant star is resolved with incredible detail, Starliner comes home empty, and amazing new images of Mercury from BepiColumbo.

Polaris Dawn launches and completes the first private spacewalk, the surface of a giant star is resolved with incredible detail, Starliner comes home empty, and amazing new images of Mercury from BepiColumbo.

Stars oscillate. Even the Sun does. And we can learn a lot about them by studying those oscillations. How is it done and what can we learn? Finding out in this interview.

Stars oscillate. Even the Sun does. And we can learn a lot about them by studying those oscillations. How is it done and what can we learn? Finding out in this interview.

Long-time Syzygy listener Jack asks: "Hey Emily — what's the deal with quasi-stars?" (We're paraphrasing). Quasi-stars are hypothetical, enormous stellar-object-thingies that might have formed shortly after the Big Bang. They're so huge they might have formed with black holes at their cores. If they existed at all, it would explain why astronomers keep finding intermediate-mass black holes in gravitational wave experiments. And as a bonus for you, Jack, Emily presents Hawking stars: otherwise ordinary stars that could be hiding a tiny black hole deep in their core. Could the Sun be a Hawking star? The mind boggles.Help us make Syzygy even better! Tell your friends and give us a review, or show your support on Patreon: patreon.com/syzygypodSyzygy is produced by Chris Stewart and co-hosted by Dr Emily Brunsden from the Department of Physics at the University of York.On the web: syzygy.fm | Instagram & Threads: @syzygypodThings we talk about in this episode:• Quasi-stars• (… as opposed to Quasars)• Types of black hole• Intermediate-mass black holes and LIGO• Hawking stars• The research paper that seeded this episode• Asteroseismology, the music of the stars

Asteroseismology of the pulsating extremely low-mass white dwarf SDSS J111215 82+111745 0: a model with p -mode pulsations consistent with the observations by Jie Su et al. on Wednesday 23 November SDSS J111215.82+111745.0 is the second pulsating extremely low-mass white dwarf discovered. Two short-period pulsations, 107.56 and 134.275 s, were detected on this star, which would be the first observed pressure mode ($p$-mode) pulsations observed on a white dwarf. While the two potential $p$-modes have yet to be confirmed, they make SDSS J111215.82+111745.0 an interesting object. In this work, we analyzed the whole set of seven periods observed on SDSS J111215.82+111745.0. We adopt three independent period-spacing tests to reveal a roughly 93.4 s mean period spacing of $ell=1$ $g$-modes, which gives added credence to the $ell=1$ identifications. Then we perform asteroseismic modeling for this star, in which the H chemical profile is taken as a variable. The stellar parameters $M=0.1650pm0.0137$ $M_odot$ and $T_mathrm{eff}=9750pm560$ K are determined from the best-fit model and the H/He chemical profiles are also defined. The two suspected $p$-modes are also well represented in the best-fit model, and both the stellar parameters and the pulsation frequencies are in good agreement with the values derived from spectroscopy. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.12011v1

Asteroseismology of the pulsating extremely low-mass white dwarf SDSS J111215 82+111745 0: a model with p -mode pulsations consistent with the observations by Jie Su et al. on Tuesday 22 November SDSS J111215.82+111745.0 is the second pulsating extremely low-mass white dwarf discovered. Two short-period pulsations, 107.56 and 134.275 s, were detected on this star, which would be the first observed pressure mode ($p$-mode) pulsations observed on a white dwarf. While the two potential $p$-modes have yet to be confirmed, they make SDSS J111215.82+111745.0 an interesting object. In this work, we analyzed the whole set of seven periods observed on SDSS J111215.82+111745.0. We adopt three independent period-spacing tests to reveal a roughly 93.4 s mean period spacing of $ell=1$ $g$-modes, which gives added credence to the $ell=1$ identifications. Then we perform asteroseismic modeling for this star, in which the H chemical profile is taken as a variable. The stellar parameters $M=0.1650pm0.0137$ $M_odot$ and $T_mathrm{eff}=9750pm560$ K are determined from the best-fit model and the H/He chemical profiles are also defined. The two suspected $p$-modes are also well represented in the best-fit model, and both the stellar parameters and the pulsation frequencies are in good agreement with the values derived from spectroscopy. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.12011v1

Pulsating H-deficient WDs and pre-WDs observed with TESS: V Discovery of two new DBV pulsators, WD J152738 4-450207 4 and WD 1708-871, and asteroseismology of the already known DBV stars PG 1351+489, EC 20058-5234, and EC 04207-4748 by Alejandro H. Córsico et al. on Wednesday 12 October The {sl TESS} space mission has recently demonstrated its great potential to discover new pulsating white dwarf and pre-white dwarf stars, and to detect periodicities with high precision in already known white-dwarf pulsators. We report the discovery of two new pulsating He-rich atmosphere white dwarfs (DBVs) and present a detailed asteroseismological analysis of three already known DBV stars employing observations collected by the {sl TESS} mission along with ground-based data. We extracted frequencies from the {sl TESS} light curves of these DBV stars using a standard pre-whitening procedure to derive the potential pulsation frequencies. All the oscillation frequencies that we found are associated with $g$-mode pulsations with periods spanning from $sim 190$ s to $sim 936$ s. We find hints of rotation from frequency triplets in some of the targets, including the two new DBVs. For three targets, we find constant period spacings, which allowed us to infer their stellar masses and constrain the harmonic degree $ell$ of the modes. We also performed period-to-period fit analyses and found an asteroseismological model for three targets, with stellar masses generally compatible with the spectroscopic masses. Obtaining seismological models allowed us to estimate the seismological distances and compare them with the precise astrometric distances measured with {it Gaia}. We find a good agreement between the seismic and the astrometric distances for three stars (PG~1351+489, EC~20058$-$5234, and EC~04207$-$4748), although for the other two stars (WD~J152738.4$-$50207 and WD~1708$-$871), the discrepancies are substantial. The high-quality data from the {sl TESS} mission continue to provide important clues to determine the internal structure of pulsating pre-white dwarf and white dwarf stars through the tools of asteroseismology. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.05486v1

Pulsating H-deficient WDs and pre-WDs observed with TESS: V Discovery of two new DBV pulsators, WD J152738 4-450207 4 and WD 1708-871, and asteroseismology of the already known DBV stars PG 1351+489, EC 20058-5234, and EC 04207-4748 by Alejandro H. Córsico et al. on Wednesday 12 October The {sl TESS} space mission has recently demonstrated its great potential to discover new pulsating white dwarf and pre-white dwarf stars, and to detect periodicities with high precision in already known white-dwarf pulsators. We report the discovery of two new pulsating He-rich atmosphere white dwarfs (DBVs) and present a detailed asteroseismological analysis of three already known DBV stars employing observations collected by the {sl TESS} mission along with ground-based data. We extracted frequencies from the {sl TESS} light curves of these DBV stars using a standard pre-whitening procedure to derive the potential pulsation frequencies. All the oscillation frequencies that we found are associated with $g$-mode pulsations with periods spanning from $sim 190$ s to $sim 936$ s. We find hints of rotation from frequency triplets in some of the targets, including the two new DBVs. For three targets, we find constant period spacings, which allowed us to infer their stellar masses and constrain the harmonic degree $ell$ of the modes. We also performed period-to-period fit analyses and found an asteroseismological model for three targets, with stellar masses generally compatible with the spectroscopic masses. Obtaining seismological models allowed us to estimate the seismological distances and compare them with the precise astrometric distances measured with {it Gaia}. We find a good agreement between the seismic and the astrometric distances for three stars (PG~1351+489, EC~20058$-$5234, and EC~04207$-$4748), although for the other two stars (WD~J152738.4$-$50207 and WD~1708$-$871), the discrepancies are substantial. The high-quality data from the {sl TESS} mission continue to provide important clues to determine the internal structure of pulsating pre-white dwarf and white dwarf stars through the tools of asteroseismology. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.05486v1

What is a starquake? On this episode, Neil deGrasse Tyson and comic co-host Matt Kirshen explore asteroseismology, the sun, and what's happening on the insides of stars with astrophysicist Conny Aerts. NOTE: StarTalk+ Patrons can listen to this entire episode commercial-free.Thanks to our Patrons Zoran Nesic, Sarah Rina Rosen, and Joshua Brewer for supporting us this week.

KIC 7955301: a hierarchical triple system with eclipse timing variations and an oscillating red giant by P. Gaulme et al. on Tuesday 11 October KIC 7955301 is a hierarchical triple system with eclipse timing and depth variations discovered by the Kepler mission. It is composed of a non-eclipsing primary star at the bottom of the red giant branch on a 209-day orbit with a K/G-type main-sequence inner eclipsing binary, orbiting in 15.3 days. This system was noted for the large amplitude of its eclipse timing variations (4 hours), and the clear solar-like oscillations of the red-giant component, including p-modes of degree up to l=3 and mixed l=1 modes. The system is a single-lined spectroscopic triple. We perform a dynamical model by combining the Kepler photometric data, eclipse timing variations, and radial-velocity data obtained at Apache Point (ARCES) and Haute Provence (SOPHIE) observatories. The dynamical mass of the red-giant is determined with a 2% precision at 1.30 (+0.03,-0.02) solar mass. We perform asteroseismic modeling based on the global seismic parameters and on the individual frequencies. Both methods lead to a mass of the red giant that matches the dynamical mass within the uncertainties. Asteroseismology also reveals the rotation rate of the core (15 days), the envelope (150 days), and the inclination (75 deg) of the red giant. Three different approaches lead to an age between 3.3 and 5.8 Gyr, which highlights the difficulty of determining stellar ages despite the exceptional wealth of available information. On short timescales, the inner binary exhibits eclipses with varying depths during a 7.3-year long interval, and no eclipses during the consecutive 11.9 years. This is why Kepler could detect its eclipses, TESS will not, and the future ESA PLATO mission should. Over the long term, the system owes its evolution to the evolution of its individual components. It could end its current smooth evolution by merging by the end of the red giant or the asymptotic giant branch of the primary star. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.05312v1

Using observations from TESS, astronomers have identified an unprecedented collection of pulsating red giant stars across the sky.

Prof. KU Leuven, Conny Aerts, is een gerenomeerd astronoom, en meer specifiek binnen haar veld 'Asteroseismology'.    We starten bij Conny haar ruimtemissie, genaamd PLATO, waarbij er ism ESA een satelliet gelanceerd zal worden om naar 'kopieën van de Aarde' te zoeken, en bijgevolg buitenaards leven. We staan natuurlijk even stil bij dat buitenaards leven en mogelijks in de ruimte te wonen.   Los daarvan hebben we het over de academische wereld, die soms krampachtig kan vasthouden aan de status quo ondanks dat nieuwe theorieën de betere waarheid blijken te bevatten.   We sluiten af met te spreken over het belang van nieuwsgierigheid en enthousiasme in ons dagelijks leven. Enjoy!   DISCOURS vzw https://www.discours.be   PODCAST Apple Podcasts: https://podcasts.apple.com/be/podcast/discours-met-de-boys/id1552090974  Spotify: https://open.spotify.com/show/1hC2t2YYCE3l7BOB12yjIr  Youtube: https://www.youtube.com/@discours SOCIALS Twitter: https://twitter.com/DiscoursDialoog  Instagram: http://instagram.com/discoursdialoog  Facebook: https://www.facebook.com/DiscoursDialoog  TikTok: https://www.tiktok.com/@discoursdialoog 

In the 1600s, many people believed the stars produced musical vibrations. While it's true stars vibrate, they don't produce any sound. Asteroseismology still uses these vibrations to learn more about the cosmos.

The instruments on NASA's TESS are ideal for studying stellar vibrations, a field of research known as asteroseismology.

NASA's TESS has given us tickets to a red giant concert in the sky.

Professor William Chaplin is a professor at the School of Physics and Astronomy at the University of Birmingham, and leads the Asteroseismology program of the NASA Kepler Mission. We’re thrilled to have Professor William Chaplin on the podcast this week to look at audio from the fascinating perspective of someone who focuses on what could be loosely termed the sound ... Read More The post EP 235 | William Chaplin appeared first on Unstoppable Recording Machine.

Cymatics holds huge potential for humanity across a wide range of scientific disciplines, everything from Asteroseismology—the study of stars from their sonic signatures--to Zoology—the study of animal calls, literally and A to Z of subjects. John Stuart Reid is an English acoustics engineer, scientist and inventor. He has studied the world of sound for over 30 years and speaks extensively on his research findings to audiences throughout the United States and the United Kingdom. Inventor of the CymaScope Pro, John's work is inspired by acoustic pioneers, Ernst Chladni, Mary D. Waller and Hans Jenny and has taken their findings to a new level. His primary interests lie in investigating sound as a formative force and discovering why sound heals.  Get more info at https://quantum.yoga/podcast-blog/qyp-46-john-stuart-reid-on-cymatics-the-visualization-of-sound-and-sound-therapy

The 14th Hintze Biannual Lecture 4th May 2017 delivered by Professor Conny Aerts - Director, Institute of Astronomy KU Leuven Thanks to the recent space missions CoRoT and Kepler, a new era of stellar physics has dawned. Asteroseismology, the observation and interpretation of starquakes, has produced a number of surprises about the deep interiors of stars. These results have altered our view of the lifecycle of stars including the generations of stars that preceded the Sun. Starquakes allow us to estimate the distances and ages of stars with unprecedented precision. Asteroseismology from space has revealed radically different physics in the heart of massive stars compared to the Sun. These massive stars are the chemical factories of the Universe, forcing us to rethink the output from the manufacturing sector of our Galaxy. Furthermore asteroseismology has paved the way for archaeological studies of our own Milky Way. After reviewing these developments I will look to the future projects that can address the new open questions posed by starquakes.

Don Kurtz, of the University of Central Lancashire, discusses asteroseismology in a lecture entitled Songs of the Stars: The Real Music of the Spheres. He explains how sound waves are helping to locate distant Earth-like planets, study solar storms and explain what happens in the core of stars.

Don Kurtz, of the University of Central Lancashire, discusses asteroseismology in a lecture entitled Songs of the Stars: The Real Music of the Spheres. He explains how sound waves are helping to locate distant Earth-like planets, study solar storms and explain what happens in the core of stars.

Don Kurtz, of the University of Central Lancashire, discusses asteroseismology in a lecture entitled Songs of the Stars: The Real Music of the Spheres. He explains how sound waves are helping to locate distant Earth-like planets, study solar storms and explain what happens in the core of stars.

Before stars burn out, they inflate to become red giants. The outer hydrogen envelope of these massive stars expand and can swallow almost anything that stands in its path, including smaller planets. Dr. Elizabeth Green, an associate astronomer at the Steward Observatory, was part of the research team that recently discovered two planets, roughly the size of Earth, that remained intact after being swallowed. During the study of the pulsations of subdwarf B star KOI 55 of the Cygnus constellation, researchers discovered that the star is, in fact, a host star that is orbited by planets KOI 55.01 and KOI 55.02. The star’s pulsations were being monitored via NASA’s Kepler telescope. French astronomer Stephane Charpinet of the Institut de Recherche en Astrophysique et Planétologie, who led the research team that discovered these planets, predicted stars would pulsate years ago. Observing a star’s pulsations can aid researchers in their quest to understand what goes on inside a star.

Wed, 30 Nov 2011 12:00:00 +0100 https://edoc.ub.uni-muenchen.de/13739/ https://edoc.ub.uni-muenchen.de/13739/1/SilvaAguirre_Victor.pdf Silva Aguirre, Victor ddc:530, ddc:500, Fakultät für Phys