Podcasts about myrs

Simultaneous gas accretion onto a pair of giant planets: Impact on their final mass and on the protoplanetary disk structure by Camille Bergez-Casalou et al. on Wednesday 30 November Several planetary systems are known to host multiple giant planets. However, when two giant planets are accreting from the same disk, it is unclear what effect the presence of the second planet has on the gas accretion process of both planets. In this paper we perform long-term 2D isothermal hydrodynamical simulations (over more than 0.5 Myrs) with the FARGO-2D1D code, considering two non-migrating planets accreting from the same gaseous disk. We find that the evolution of the planets' mass ratio depends on gap formation. However, in all cases, when the planets start accreting at the same time, they end up with very similar masses (0.9 $

Merger Signatures are Common, but not Universal, In Massive, Recently-Quenched Galaxies at z~0 7 by Margaret Verrico et al. on Wednesday 30 November We present visual classifications of merger-induced tidal disturbances in 143 $rm{M}_* sim 10^{11}rm{M}_odot$ post-starburst galaxies at z$sim$0.7 identified in the SQuIGG$vec{L}$E Sample. This sample spectroscopically selects galaxies from the Sloan Digital Sky Survey that have stopped their primary epoch of star formation within the past $sim$500 Myrs. Visual classifications are performed on Hyper Suprime Cam (HSC) i-band imaging. We compare to a control sample of mass- and redshift-matched star-forming and quiescent galaxies from the Large Early Galaxy Census and find that post-starburst galaxies are more likely to be classified as disturbed than either category. This corresponds to a factor of $3.6^{+2.9}_{-1.3}$ times the disturbance rate of older quiescent galaxies and $2.1^{+1.9}_{-.73}$ times the disturbance rate of star-forming galaxies. Assuming tidal features persist for $lesssim500$ Myr, this suggests merging is coincident with quenching in a significant fraction of these post-starbursts. Galaxies with tidal disturbances are younger on average than undisturbed post-starburst galaxies in our sample, suggesting tidal features from a major merger may have faded over time. This may be exacerbated by the fact that, on average, the undisturbed subset is fainter, rendering low surface brightness tidal features harder to identify. However, the presence of ten young ($lesssim150$ Myr since quenching) undisturbed galaxies suggests that major mergers are not the only fast physical mechanism that shut down the primary epoch of star formation in massive galaxies at intermediate redshift. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.16532v1

Merger Signatures are Common, but not Universal, In Massive, Recently-Quenched Galaxies at z~0 7 by Margaret Verrico et al. on Wednesday 30 November We present visual classifications of merger-induced tidal disturbances in 143 $rm{M}_* sim 10^{11}rm{M}_odot$ post-starburst galaxies at z$sim$0.7 identified in the SQuIGG$vec{L}$E Sample. This sample spectroscopically selects galaxies from the Sloan Digital Sky Survey that have stopped their primary epoch of star formation within the past $sim$500 Myrs. Visual classifications are performed on Hyper Suprime Cam (HSC) i-band imaging. We compare to a control sample of mass- and redshift-matched star-forming and quiescent galaxies from the Large Early Galaxy Census and find that post-starburst galaxies are more likely to be classified as disturbed than either category. This corresponds to a factor of $3.6^{+2.9}_{-1.3}$ times the disturbance rate of older quiescent galaxies and $2.1^{+1.9}_{-.73}$ times the disturbance rate of star-forming galaxies. Assuming tidal features persist for $lesssim500$ Myr, this suggests merging is coincident with quenching in a significant fraction of these post-starbursts. Galaxies with tidal disturbances are younger on average than undisturbed post-starburst galaxies in our sample, suggesting tidal features from a major merger may have faded over time. This may be exacerbated by the fact that, on average, the undisturbed subset is fainter, rendering low surface brightness tidal features harder to identify. However, the presence of ten young ($lesssim150$ Myr since quenching) undisturbed galaxies suggests that major mergers are not the only fast physical mechanism that shut down the primary epoch of star formation in massive galaxies at intermediate redshift. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.16532v1

Simultaneous gas accretion onto a pair of giant planets: Impact on their final mass and on the protoplanetary disk structure by Camille Bergez-Casalou et al. on Wednesday 30 November Several planetary systems are known to host multiple giant planets. However, when two giant planets are accreting from the same disk, it is unclear what effect the presence of the second planet has on the gas accretion process of both planets. In this paper we perform long-term 2D isothermal hydrodynamical simulations (over more than 0.5 Myrs) with the FARGO-2D1D code, considering two non-migrating planets accreting from the same gaseous disk. We find that the evolution of the planets' mass ratio depends on gap formation. However, in all cases, when the planets start accreting at the same time, they end up with very similar masses (0.9 $

Growth of A Massive Black Hole Via Tidal Disruption Accretion by Seungjae Lee et al. on Wednesday 30 November Stars that are tidally disrupted by the massive black hole (MBH) may contribute significantly to the growth of the MBH, especially in dense nuclear star clusters (NSCs). Yet, this tidal disruption accretion (TDA) of stars onto the MBH has largely been overlooked compared to the gas accretion (GA) channel in most numerical experiments until now. In this work, we implement a black hole growth channel via TDA in the high-resolution adaptive mesh refinement code Enzo to investigate its influence on a MBH seed's early evolution. We find that a MBH seed grows rapidly from $10^3,mathrm{M}_odot$ to $gtrsim 10^6,mathrm{M}_odot$ in 200,Myrs in some of the tested simulations. Compared to a MBH seed that grows only via GA, TDA can enhance the MBH's growth rate by up to more than an order of magnitude. However, as predicted, TDA mainly helps the early growth of the MBH (from $10^{3-4},mathrm{M}_odot$ to $lesssim10^{5},mathrm{M}_odot$) while the later evolution is generally dominated by GA. We also observe that the star formation near the MBH is suppressed when TDA is most active, sometimes with a visible cavity in gas (of size $sim$ a few pc) created in the vicinity of the MBH. It is because the MBH may grow expeditiously with both GA and TDA, and the massive MBH could consume its neighboring gas faster than being replenished by gas inflows. Our study demonstrates the need to consider different channels of black hole accretion that may provide clues for the existence of supermassive black holes at high redshifts. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.02376v2

Simultaneous gas accretion onto a pair of giant planets: Impact on their final mass and on the protoplanetary disk structure by Camille Bergez-Casalou et al. on Wednesday 30 November Several planetary systems are known to host multiple giant planets. However, when two giant planets are accreting from the same disk, it is unclear what effect the presence of the second planet has on the gas accretion process of both planets. In this paper we perform long-term 2D isothermal hydrodynamical simulations (over more than 0.5 Myrs) with the FARGO-2D1D code, considering two non-migrating planets accreting from the same gaseous disk. We find that the evolution of the planets' mass ratio depends on gap formation. However, in all cases, when the planets start accreting at the same time, they end up with very similar masses (0.9 $

Simultaneous gas accretion onto a pair of giant planets: Impact on their final mass and on the protoplanetary disk structure by Camille Bergez-Casalou et al. on Wednesday 30 November Several planetary systems are known to host multiple giant planets. However, when two giant planets are accreting from the same disk, it is unclear what effect the presence of the second planet has on the gas accretion process of both planets. In this paper we perform long-term 2D isothermal hydrodynamical simulations (over more than 0.5 Myrs) with the FARGO-2D1D code, considering two non-migrating planets accreting from the same gaseous disk. We find that the evolution of the planets' mass ratio depends on gap formation. However, in all cases, when the planets start accreting at the same time, they end up with very similar masses (0.9 $

Growth of A Massive Black Hole Via Tidal Disruption Accretion by Seungjae Lee et al. on Tuesday 29 November Stars that are tidally disrupted by the massive black hole (MBH) may contribute significantly to the growth of the MBH, especially in dense nuclear star clusters (NSCs). Yet, this tidal disruption accretion (TDA) of stars onto the MBH has largely been overlooked compared to the gas accretion (GA) channel in most numerical experiments until now. In this work, we implement a black hole growth channel via TDA in the high-resolution adaptive mesh refinement code Enzo to investigate its influence on a MBH seed's early evolution. We find that a MBH seed grows rapidly from $10^3,mathrm{M}_odot$ to $gtrsim 10^6,mathrm{M}_odot$ in 200,Myrs in some of the tested simulations. Compared to a MBH seed that grows only via GA, TDA can enhance the MBH's growth rate by up to more than an order of magnitude. However, as predicted, TDA mainly helps the early growth of the MBH (from $10^{3-4},mathrm{M}_odot$ to $lesssim10^{5},mathrm{M}_odot$) while the later evolution is generally dominated by GA. We also observe that the star formation near the MBH is suppressed when TDA is most active, sometimes with a visible cavity in gas (of size $sim$ a few pc) created in the vicinity of the MBH. It is because the MBH may grow expeditiously with both GA and TDA, and the massive MBH could consume its neighboring gas faster than being replenished by gas inflows. Our study demonstrates the need to consider different channels of black hole accretion that may provide clues for the existence of supermassive black holes at high redshifts. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.02376v2

Early Results From GLASS-JWST XII: The Morphology of Galaxies at the Epoch of Reionization by T. Treu et al. on Monday 19 September Star-forming galaxies can exhibit strong morphological differences between the rest-frame far-UV and optical, reflecting inhomogeneities in star-formation and dust attenuation. We exploit deep, high resolution NIRCAM 7-band observations to take a first look at the morphology of galaxies in the epoch of reionization ($z>7$), and its variation in the rest-frame wavelength range between Lyman $alpha$ and 6000-4000AA, at $z=7-12$. We find no dramatic variations in morphology with wavelength -- of the kind that would have overturned anything we have learned from the Hubble Space Telescope. No significant trends between morphology and wavelengths are detected using standard quantitative morphology statistics. We detect signatures of mergers/interactions in 4/19 galaxies. Our results are consistent with a scenario in which Lyman Break galaxies -- observed when the universe is only 400-800 Myrs old - are growing via a combination of rapid galaxy-scale star formation supplemented by accretion of star forming clumps and interactions. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2207.13527v2

Fundamentals of Stellar Parameters Estimation through CMD of Star Clusters: Open NGC2360 and Globular NGC 5272 by Kanwar Preet Kaur et al. on Wednesday 07 September The fundamentals of estimating essential stellar parameters of an open cluster-NGC 2360 and globular clusters-NGC 5272 are presented extensively in this work. Here, the evaluation of stellar parameters, by manually fitting the appropriate isochrones on the color magnitude diagrams (CMDs), of the selected star clusters is discussed comprehensively. Aperture photometry and PSF fitting photometry are conducted on g, r, and i standard band filter images of Sloan Digital Sky Survey (SDSS) using the aperture photometry tool (APT) to obtain the respective CMDs. Further, to achieve the stellar parameters, isochrone fitting is described in detail. This work on stellar parameters evaluation has attained the following results: age of NGC 2360 is found to be 708 Myrs with metallicity, [Fe/H], of -0.15, whereas NGC 5272 is having age of 11.56 Gyrs with metallicity, [Fe/H], of -1.57. Additionally, the interstellar reddening, E(B-V), and distance modulus, DM, for NGC 2360 are obtained as 0.12 and 11.65, respectively. While, for NGC 5272, the interstellar reddening is attained as E(B-V)=0.015, and the distance modulus is DM=15.1. The values of these stellar parameters are found to be in close approximation with the results provided in the literature based on the IRAF analysis technique. The distribution of radii, masses, and temperatures are included along with the initial mass function (IMF) for both the start clusters. Thus, this article would aid in providing insight into the evaluation of stellar parameters by the astronomical photometry analysis which would successively upsurge the understanding of our universe. It should be noted that the cleaning of cluster population on the CMDs from the foreground/background stars, clearing of spurious objects, error estimations and the membership determination are not carried out in this work and are considered as separate project for analysis. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.03019v1

Ultramassive black holes formed by triple quasar mergers at z sim 2 by Yueying Ni et al. on Wednesday 07 September The origin of rare and elusive ultramassive black holes (UMBH, with MBH > 1e10 Msun) is an open question. Using the large volume cosmological hydrodynamic simulation ASTRID, we report on the formation of an extremely massive UMBH with MBH ~ 1e11 Msun at z~2. The UMBH is assembled as a result of two successive mergers of massive galaxies each with stellar mass M* > 3e11 Msun that also produces a bright, rare triple quasar system powered by three ~10^9 Msun black holes. The second merger of supermassive black holes (SMBHs) follows the first after 150 Myrs. The merger events lead to sustained Eddington accretion onto the central SMBH, forming an UMBH in the center of a massive compact stellar core with M* > 2e12 Msun. The strong feedback of the UMBH quenches the surrounding star formation to < 10 Msun/yr in the inner 50 kpc/h region. There are two more UMBHs with MBH > 5e10 Msun at z>2 in ASTRID which are also produced by major mergers of galaxies, and their progenitors can be observed as quasar triplets of lower luminosity. The rarely observed quasar multiples can be the cradle of UMBHs at high redshift, and likely end up in the center of the most massive clusters. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.01249v2

On this episode of the podcast we caught up with Brain De Wild, a multi-instrumentalist and songwriter making vintage sounding psych & prog rock. We chat about the process of writing and recording the song ‘Moby Dick’, some of his influences and more. Follow folks @briandewild @StudyMusicGroup @ctznofficial • Music between the intro segments: Low Hiss (‘Untitled #8’), an outtake from the demo version of his album EP-303. Mix Tracklist: 1. Gee & CTZN - half baked 2. Las Dos - Roots & Herbs 3. HMZA. - Arab Cobain 4. thegoodnews. - Sometimes (feat. MYRS) 5. Black Aesop - Fast Actin' (feat. Walt Liquor) 6. CTZN - nogimics • studymusicgroup.com/podcast • --- This episode is sponsored by · Anchor: The easiest way to make a podcast. https://anchor.fm/app --- Send in a voice message: https://anchor.fm/studymusicgroup/message Support this podcast: https://anchor.fm/studymusicgroup/support

This week we dive into a Myrs life! With token Brudiclad. MYR.png 748 KB The Deck:https://archidekt.com/decks/717580#myrEmailwolfystar12@gmail.com Twitter@wolfymtgMusic: https://www.bensound.com

Happy 4/20 week, hope everybody is getting along as well as possible, all things considered. • On today’s episode we’re debuting new music from thegoodnews. (@notpo3 @ctznofficial @petecosmos) • “...The One For $20” follows the groups 2016 self-titled album and is the first in a collection of new works the group has been preparing in the time since. Added a bonus b-side joint here also, ‘Sometimes (The Zone)’ featuring El Paso, TX composer/producer MYRS. --- This episode is sponsored by · Anchor: The easiest way to make a podcast. https://anchor.fm/app Support this podcast: https://anchor.fm/studymusicgroup/support

Looks Like A Lawsuit, Batman! - A mix of original music, beats and remixes from El Paso, TX producer MYRS, featuring CTZN & Sergio Franco. Check out his most recent instrumental album "The Gateway To Immortality", and his compilation album featuring The Understudies Crew "Sound Pictures of The Future". @jacobmyers213 @ctznofficial @studymusicgroup StudyMusicGroup.com --- This episode is sponsored by · Anchor: The easiest way to make a podcast. https://anchor.fm/app Support this podcast: https://anchor.fm/studymusicgroup/support

Energized by her victory in the Cube Draft, Amber once again seizes the reins of her scrap destiny to try to make a clean sweep. Kenny, however, won’t go quietly into that good magic night. He’s pulling out all the stops, leveraging the power of Teferi, Temporal Archmage, in a monoblue superfriends grindfest of a Commander deck. It’s planeswalker vs. planeswalker in this battle royale featuring giant spells from both sides of the table. Monored. Monoblue. Only one will emerge victorious. The post Poopin’ Out Myrs appeared first on Geekspective.

Трагично и энергично (Russian Dance House) 1. Серебро - Пятница 2. Настя Задорожная - Я больше не хочу верить 3. Зомб - Горит на танцполе 4. Amanda - Полюбила друга 5. Myrs - Танцуй 6. Дима Билан - Молния 7. Оля Краснова - Слишком хорош 8. неизвестен 9. Dante - Не вздумай 10. Александр Панайотов - Ночь на облаках 11. Dabro - Между нами ток 12. Ворона - Пудра 13. неизвестен 14. неизвестен 15. Иван Валеев - Танцуй со мной 16. Karaty feat Ika - Hey, DJ

This thesis is divided into two parts: an instrumentation part and an astrophysical part. The instrumentation part describes the development and implementation of the fiber coupler and guiding subsystems of the 2nd generation VLTI instrument GRAVITY. The astrophysical part describes the derivation of the star formation history of the Milky Way’s nuclear star cluster based on imaging and spectroscopic data obtained at the Very Large Telescope. The future VLTI instrument GRAVITY will deliver micro-arcsecond astrometry, using the interferometric combination of four telescopes. The instrument is a joint project of several European institutes lead by the Max Planck Institut f¨ur extraterrestrische Physik. The instrumental part of this thesis describes the fiber coupler unit and the guiding system. They serve for beam stabilization and light injection in GRAVITY. In order to deliver micro-arcsecond astrometry, GRAVITY requires an unprecedented stability of the VLTI optical train. We therefore developed a dedicated guiding system, correcting the longitudinal and lateral pupil wanderas well as the image jitter in VLTI tunnel. The actuators for the correction are provided by four fiber coupler units located in the GRAVITY cryostat. Each fiber coupler picks the light of one telescope and stabilizes the beam. Furthermore each unit provides field de-rotation, polarization adjustment as well as atmospheric piston correction. A novel roof-prism design offers the possibility of on-axis as well as off-axis fringe tracking. Finally the stabilized beam is injected with minimized losses into singlemode fibers via parabolic mirrors. We present lab results of the first guiding- as well as the first fiber coupler prototype, in particular the closed loop performance and the optical quality. Based on the lab results we derive the on-sky performance of the systems and the implications concerning the sensitivity of GRAVITY. The astrophysical part of this thesis presents imaging and integral field spectroscopy data for 450 cool giant stars within 1 pc from Sgr A*. We use the prominent CO bandheads to derive effective temperatures of individual giants. Additionally we present the deepest spectroscopic observation of the Galactic Center so far, probing the number of B9/A0 main sequence stars (2.2 − 2.8M) in two deep fields. From spectro-photometry we construct a Hertzsprung-Russell diagram of the red giant population and fit the observed diagram with model populations to derive the star formation history of the nuclear cluster. We find that (1) the average nuclear star-formation rate dropped from an initial maximum 10Gyrs ago to a deep minimum 1-2Gyrs ago and increased again during the last few hundred Myrs, and (2) that roughly 80% of the stellar mass formed more than 5Gyrs ago; (3) mass estimates within R 1 pc from Sgr A* favor a dominant star formation mode with a normal Chabrier/Kroupa initial mass function for the majority of the past star formation in the Galactic Center. The bulk stellar mass seems to have formed under conditions significantly different from the observed young stellar disks, perhaps because at the time of the formation of the nuclear cluster the massive black hole and its sphere of influence was much smaller than today.

Young stars close to the sun (within 100 pc) yield an interesting sample in many respects: They are relatively bright and because of their close distance we can resolve the surroundings of these stars by using adaptive optics on 8 to 10 m class telescopes (e.g. VLT or Keck). In the K-band the achievable angular resolution is about 50 mas which corresponds to 5 AU at a star closer than 100 pc; 5 AU is about the distance between the Sun and Jupiter. This possibility can be used to study surrounding material such as disks made up of gas and dust as well as stellar and substellar companions. A sample consisting of young stars in the solar vicinity and in an evolutionary stage between the classical T Tauri phase with a disk and the zero-age main sequence can be provided by the catalog of flare stars and related objects compiled by Gershberg et al. (1999) because young stars are often variable and exhibit large eruptions (flares). In a first step we need to verify that these stars are indeed young and did not come to lie above the main sequence in a Hertzsprung-Russell diagram because they are old or unresolved binaries or multiples. Therefore, we have taken spectra of 223 stars lying above the main sequence (of the 463 stars of the sample). The distances to these stars were measured (in most cases by Hipparcos) and they are located at a few to 100 pc. The goal was to detect lithium absorption at 6708 A which all young stars have in common. In addition to the detection of lithium, we want to identify other age indicators such as filling in or emission of the Halpha -, the magnesium Ib- and the calcium lines. The G- and K-type stars of the northern hemisphere were also observed with high resolution, and high signal-to-noise ratio spectroscopy to study these objects with methods of spectral synthesis analysis to determine the surface gravity, the chemical composition, and the temperature. The age determination of these 223 stars lead to a value between 10 Myr and the zero-age main sequence, they are indeed nearby and 17 stars are clearly pre-main sequence. In the course of this work, we discovered the closest pre-main sequence star (HIP 108405 A, 10+-10 Myrs at a distance of 16.1pc). The star is younger than GJ 182 (27 pc, 20+-10 Myrs) which held the record up to now. A planet with a mass of 5 MJup in orbit of a (for this sample) typical M-star, would have an apparent magnitude in the K-band of 14.5 to 17.5 mag at a distance of 16 pc. This would lead to a magnitude difference DeltaK of 8 to 11 mag between the star and the companion, which could be detected with 8 to 10 m class telescopes at a separation of 1" or a projected separation of 16 AU. All newly discovered young flare stars were imaged using NAOS/CONICA to search for distant companions. Depending on the space motion of the stars, they have to be reobserved in one or more years to distinguish comoving companions from stagnant background stars. In this work we have measured radial velocity variations of young stars for the first time using the échelle spectrograph of the Thüringer Landessternwarte. In these measurements one can see the problems of such an investigation, such as variability caused by activity and stellar spots. But one can also see that it is in principle possible to detect planets around active young stars. To verify the results and to measure longer rotation periods, we have to observe these stars for another season.