Gotowe bibliografie tematyczne / Accretion; gravitational

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Gotowa bibliografia na temat „Accretion; gravitational”

Autor: Grafiati

Data publikacji: 3 czerwca 2025

Data aktualizacji: 31 lipca 2025

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Artykuły w czasopismach na temat "Accretion; gravitational"

Cattorini, Federico, Sofia Maggioni, Bruno Giacomazzo, Francesco Haardt, Monica Colpi, and Stefano Covino. "Misaligned Spinning Binary Black Hole Mergers in Hot Magnetized Plasma." Astrophysical Journal Letters 930, no. 1 (2022): L1. http://dx.doi.org/10.3847/2041-8213/ac6755.

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Abstract We present general relativistic magnetohydrodynamical simulations of equal-mass spinning black hole binary mergers embedded in a magnetized gas cloud. We focus on the effect of the spin orientation relative to the orbital angular momentum on the flow dynamics, mass accretion rate, and Poynting luminosity. We find that, across the inspiral, the gas accreting onto the individual black holes concentrates into disklike overdensities whose angular momenta are oriented toward the spin axes and that persist until merger. We identify quasiperiodic modulations occurring in the mass accretion r

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BOGOVALOV, S. V., and S. R. KELNER. "ACCRETION AND PLASMA OUTFLOW FROM DISSIPATIONLESS DISCS." International Journal of Modern Physics D 19, no. 03 (2010): 339–65. http://dx.doi.org/10.1142/s0218271810016373.

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We consider the specific case of disc accretion for negligibly low viscosity and infinitely high electric conductivity. The key component in this model is the outflowing magnetized wind from the accretion disc, since this wind effectively carries away angular momentum of the accreting matter. Assuming magnetic field has variable polarity in the disc (to avoid magnetic flux and energy accumulation at the gravitational center), this leads to radiatively inefficient accretion of the disc matter onto the gravitational center. In such a case, the wind forms an outflow, which carries away all the en

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Lau, Mike Y. M., Ryosuke Hirai, Ilya Mandel, and Christopher A. Tout. "Expansion of Accreting Main-sequence Stars during Rapid Mass Transfer." Astrophysical Journal Letters 966, no. 1 (2024): L7. http://dx.doi.org/10.3847/2041-8213/ad3d50.

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Abstract Accreting main-sequence stars expand significantly when the mass accretion timescale is much shorter than their thermal timescales. This occurs during mass transfer from an evolved giant star onto a main-sequence companion in a binary system and is an important phase in the formation of compact binaries including X-ray binaries, cataclysmic variables, and gravitational-wave sources. In this study, we compute 1D stellar models of main-sequence accretors with different initial masses and accretion rates. The calculations are used to derive semianalytical approximations to the maximum ex

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Rehman, H., and G. Abbas. "Accretion around a hairy black hole in the framework of gravitational decoupling theory." Chinese Physics C 47, no. 12 (2023): 125106. http://dx.doi.org/10.1088/1674-1137/ad010e.

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Abstract We investigate astrophysical accretion onto a static and spherically symmetric hairy black hole within the framework of gravitational decoupling. To achieve this goal, we examine the accretion procedure for several types of perfect fluids, including polytropic fluid and ultra-stiff, ultra-relativistic, radiation, and sub-relativistic isothermal fluids. Moreover, we determine the critical or sonic points for numerous fluid forms that are accreting onto the black hole by utilizing the Hamiltonian dynamical approach. Additionally, the closed form of the solutions are presented for a numb

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Gittins, Fabian, and Nils Andersson. "Population synthesis of accreting neutron stars emitting gravitational waves." Monthly Notices of the Royal Astronomical Society 488, no. 1 (2019): 99–110. http://dx.doi.org/10.1093/mnras/stz1719.

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ABSTRACT The fastest-spinning neutron stars in low-mass X-ray binaries, despite having undergone millions of years of accretion, have been observed to spin well below the Keplerian break-up frequency. We simulate the spin evolution of synthetic populations of accreting neutron stars in order to assess whether gravitational waves can explain this behaviour and provide the distribution of spins that is observed. We model both persistent and transient accretion and consider two gravitational-wave-production mechanisms that could be present in these systems: thermal mountains and unstable rmodes.

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Toscani, Martina, Giuseppe Lodato, and Rebecca Nealon. "Gravitational wave emission from unstable accretion discs in tidal disruption events." Monthly Notices of the Royal Astronomical Society 489, no. 1 (2019): 699–706. http://dx.doi.org/10.1093/mnras/stz2201.

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Abstract Gravitational waves can be emitted by accretion discs if they undergo instabilities that generate a time varying mass quadrupole. In this work we investigate the gravitational signal generated by a thick accretion disc of 1 M⊙ around a static supermassive black hole of 106 M⊙, assumed to be formed after the tidal disruption of a solar type star. This torus has been shown to be unstable to a global non-axisymmetric hydrodynamic instability, the Papaloizou–Pringle instability, in the case where it is not already accreting and has a weak magnetic field. We start by deriving analytical es

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Heigl, S., A. Burkert, and M. Gritschneder. "Accretion-driven turbulence in filaments – I. Non-gravitational accretion." Monthly Notices of the Royal Astronomical Society 474, no. 4 (2017): 4881–93. http://dx.doi.org/10.1093/mnras/stx3145.

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Townsley, Dean M., and Lars Bildsten. "Physical Interpretation of Dwarf Nova Primary Effective Temperatures." International Astronomical Union Colloquium 194 (2004): 192–93. http://dx.doi.org/10.1017/s0252921100152431.

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AbstractWe have undertaken a theoretical study of the impact of the accumulating envelopes on the thermal state of the underlying white dwarf (WD). This has allowed us to find the equilibrium WD core temperatures, the classical nova ignition masses and the thermal luminosities for WDs accreting at rates of 10–11 – 10–8M⊙ yr–1. These accretion rates are most, appropriate to WDs in cataclysmic variables (CVs) of (Porb ≲ 7 hr), many of which accrete sporadically as Dwarf Novae. Over twenty Dwarf Novae have been observed in quiescence, when the accretion rate is low and the WD photosphere is detec

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BECERRA, L. M., J. A. RUEDA, and R. RUFFINI. "SPH simulations of the induced gravitational collapse." Astronomical and Astrophysical Transactions, Volume 33, Numéro 3 (December 15, 2022): 265–72. http://dx.doi.org/10.17184/eac.7529.

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In the induced gravitational collapse (IGC) paradigm, a carbon–oxygen (CO) star collapses and explodes in a supernova (SN) in the presence of a binary companion, a neutron star (NS). The material ejected in the explosion is gravitationally attracted by the NS, triggering a hypercritical accretion process onto it. For compact systems, the accretion rate could be high enough for the NS to reach its critical mass, collapse in a black hole (BH) and emit an energetic (energy release $\gtrsim 10^{52}$ erg) gamma-ray burst (GRB). With the aim to identify the separatrix of systems in which a BH is for

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Horák, Jiří, and Vladimír Karas. "Intensity and polarization light-curves from radiatively-driven clouds." Proceedings of the International Astronomical Union 2, S238 (2006): 381–82. http://dx.doi.org/10.1017/s1743921307005558.

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AbstractWe study linear polarization from scattering of light on a cloud of relativistic electrons. We assume that the cloud is hovering above an accretion disc, or it is in an accelerated motion underthe combined influence of the radiation and gravitational fields near an accreting black hole. Atfirst we derive simple and general analytical formulae for the Stokes parameters. These formulae are then used in calculations of the temporal evolution of the observed signal.We find that higher-order images can significantly enhance the observed flux. Possible targets where the effect should be sear

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Rozprawy doktorskie na temat "Accretion; gravitational"

Schneck, Kristiana E. (Kristiana Elizabeth). "Gravitational influences on magnetic field structure in accretion disks." Thesis, Massachusetts Institute of Technology, 2010. http://hdl.handle.net/1721.1/61266.

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Thesis (S.B.)--Massachusetts Institute of Technology, Dept. of Physics, 2010.<br>Cataloged from PDF version of thesis.<br>Includes bibliographical references (p. 53).<br>Black holes and compact objects are often surrounded by structures known as accretion disks which consist of ionized plasma. Due to the immense forces present in the disk, interesting and complex magnetic field structures can be set up within the disk. The influence of gravity on these structures is explored via a higher-order expansion of the gravitational potential. We consider several cases: the case when the Lorentz force

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Lin, Min-Kai, and Kaitlin M. Kratter. "ON THE GRAVITATIONAL STABILITY OF GRAVITO-TURBULENT ACCRETION DISKS." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621384.

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Low mass, self-gravitating accretion disks admit quasi-steady, "gravito-turbulent" states in which cooling balances turbulent viscous heating. However, numerical simulations show that gravito-turbulence cannot be sustained beyond dynamical timescales when the cooling rate or corresponding turbulent viscosity is too large. The result is disk fragmentation. We motivate and quantify an interpretation of disk fragmentation as the inability to maintain gravito-turbulence due to formal secondary instabilities driven by: (1) cooling, which reduces pressure support; and/or (2) viscosity, which reduces

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Britsch, Markward. "Gravitational instability and fragmentation of self-gravitating accretion disks." [S.l. : s.n.], 2006. http://nbn-resolving.de/urn:nbn:de:bsz:16-opus-69667.

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Poindexter, Shawn David. "Sharpening The Tools of Gravitational Microlensing." The Ohio State University, 2009. http://rave.ohiolink.edu/etdc/view?acc_num=osu1258766992.

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Morgan, Christopher Warren. "Quasar Structure from Microlensing in Gravitationally Lensed Quasars." The Ohio State University, 2008. http://rave.ohiolink.edu/etdc/view?acc_num=osu1205848751.

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Britsch, Markward [Verfasser], and Wolfgang [Akademischer Betreuer] Duschl. "Gravitational instability and fragmentation of self-gravitating accretion disks / Markward Britsch ; Betreuer: Wolfgang Duschl." Heidelberg : Universitätsbibliothek Heidelberg, 2006. http://d-nb.info/1178678075/34.

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Brown, Jacqueline. "Surging Seepage: A Triple Bond Accretion System." VCU Scholars Compass, 2008. http://scholarscompass.vcu.edu/etd/1481.

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My current work revels in a state of flux. I strive for the work to be electrically charged, conveying a feverish sense of immediacy and vitality that implies motion and frenetic energy. The work is an accretion of brightly colored biomorphic forms that extend out from the wall and onto the floor. Viscous parts ooze and drip while others are globular and bulbous. The hyper-organic forms suggest a paradoxical state of both ripening and rotting, becoming and unbecoming. The work is an attempt to traverse between seemingly divergent constructs, some of which include: growth and decay, the artifi

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Feltre, Anna. "Multi-band Emission of Active Galactic Nuclei: the Relationship of Stellar and Gravitational-Accretion Activity." Doctoral thesis, Università degli studi di Padova, 2013. http://hdl.handle.net/11577/3423457.

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One of the remaining open issues in the context of the analysis of active galactic nuclei is the evidence that nuclear gravitational accretion is often accompanied by a concurrent starburst activity. What is, in this picture, the role played by the obscuring dust around the nucleus and what does the state of the art models have to say? Can the infrared data provided by Spitzer and Herschel help us in extensively investigate both phenomena and, if so, how and with what limitations? Does the presence of an active nucleus have an impact in the mid- and far-infrared properties of galaxies? Which a

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TOSCANI, MARTINA. "TIDAL DISRUPTION EVENTS IN THE ERA OF MULTIMESSENGER ASTRONOMY." Doctoral thesis, Università degli Studi di Milano, 2021. http://hdl.handle.net/2434/874970.

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Tidal Disruption Events (TDEs) occur when a star, wandering too close to a black hole (BH), is torn apart by BH tides. After the disruption, roughly half of the stellar debris is expected to circularize around the BH and eventually form an accretion disc. These events represent a unique way to detect BHs through the universe since they emit both electromagnetic (EM) radiation and gravitational waves (GWs). In fact, after returning to the pericenter, the stellar material accretes onto the central object, producing very luminous EM flares. To date, around 50 robust TDEs have been detected in di

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Stone, Nicholas Chamberlain. "Tidal Disruption of Stars by Supermassive Black Holes." Thesis, Harvard University, 2013. http://dissertations.umi.com/gsas.harvard:10998.

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This thesis presents theoretical results on the tidal disruption of stars by supermassive black holes (SMBHs). The multiwavelength ares produced by tidal disruption events (TDEs) have supernova-like luminosities, and associated relativistic jets can be visible to cosmological distances. TDEs probe the demography of quiescent SMBHs, and are natural laboratories for jet launching mechanisms and super-Eddington accretion. The first chapter broadly surveys TDE physics. The second and third chapters estimate the TDE rate following gravitational wave (GW) recoil of a SMBH (after a SMBH binary merger

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Książki na temat "Accretion; gravitational"

Hartmann, Lee. Accretion processes in star formation. 2nd ed. Cambridge University Press, 2009.

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United States. National Aeronautics and Space Administration., ed. EUVE spectroscopy of the accretion region in AM Herculis: Final technical report for NAG 5-2991, report period: 15 July 1996 - 14 July 1997. National Aeronautics and Space Administration, 1997.

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Tamburini, Fabrizio. Aspects of gravitation in astrophysics: From accretion disks to quantum astronomy. University of Portsmouth, Institute of Cosmology and Gravitation, 2002.

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Hartmann, Lee. Accretion Processes in Star Formation. Cambridge University Press, 2004.

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MHD flows in compact astrophysical objects: Accretion, winds and jets. Springer, 2010.

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Trieloff, Mario. Noble Gases. Oxford University Press, 2017. http://dx.doi.org/10.1093/acrefore/9780190647926.013.30.

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This is an advance summary of a forthcoming article in the Oxford Encyclopedia of Planetary Science. Please check back later for the full article.Although the second most abundant element in the cosmos is helium, noble gases are also called rare gases. The reason is that they are not abundant on terrestrial planets like our Earth, which is characterized by orders of magnitude depletion of—particularly light—noble gases when compared to the cosmic element abundance pattern. Indeed, such geochemical depletion and enrichment processes make noble gases so versatile concerning planetary formation a

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Części książek na temat "Accretion; gravitational"

Wiita, Paul J. "Accretion Disks Around Black Holes." In Black Holes, Gravitational Radiation and the Universe. Springer Netherlands, 1999. http://dx.doi.org/10.1007/978-94-017-0934-7_16.

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Mewes, Vassilios, Pedro J. Montero, Nikolaos Stergioulas, Filippo Galeazzi, and José A. Font. "General Relativistic Simulations of Accretion Disks Around Tilted Kerr Black Holes." In Gravitational Wave Astrophysics. Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-10488-1_10.

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Meier, David L. "The Combustion Chamber: Energy Generation by Gravitational Accretion." In Black Hole Astrophysics. Springer Berlin Heidelberg, 2012. http://dx.doi.org/10.1007/978-3-642-01936-4_12.

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Cowsik, R. "Energetic Photon Spectra as Probes of the Process of Particle Acceleration in Accretion Flows Around Black Holes." In Black Holes, Gravitational Radiation and the Universe. Springer Netherlands, 1999. http://dx.doi.org/10.1007/978-94-017-0934-7_19.

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Lynden-Bell, D. "Accretion and Collapse." In Gravitation in Astrophysics. Springer US, 1987. http://dx.doi.org/10.1007/978-1-4613-1897-2_4.

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Kuperus, M. "Accretion Disk Electrodynamics." In Gravitation in Astrophysics. Springer US, 1987. http://dx.doi.org/10.1007/978-1-4613-1897-2_5.

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Bailyn, Charles D. "Accretion onto a Black Hole." In What Does a Black Hole Look Like? Princeton University Press, 2014. http://dx.doi.org/10.23943/princeton/9780691148823.003.0002.

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This chapter explores the ways that accretion onto a black hole produces energy and radiation. As material falls into a gravitational potential well, energy is transformed from gravitational potential energy into other forms of energy, so that total energy is conserved. Observing such accretion energy is one of the primary ways that astrophysicists pinpoint the locations of potential black holes. The spectrum and intensity of this radiation is governed by the geometry of the gas flow, the mass infall rate, and the mass of the accretor. The simplest flow geometry is that of a stationary object

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Moffat, John W. "Early Observations of Black Holes." In The Shadow of the Black Hole. Oxford University Press, 2020. http://dx.doi.org/10.1093/oso/9780190650728.003.0004.

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Early observations of black holes, before the LIGO/Virgo detection of gravitational waves, were made by observing electromagnetic processes involving atomic spectral lines. X-ray binary systems were observed consisting of a progenitor star such as a neutron star and a dark companion. X-rays emitted from the gas accreting the dark companion tells us whether it is a black hole. Evidence indicated supermassive black holes at the centers of galaxies. From observations of orbits of stars near the supermassive black holes, one could determine their masses, which proved they were black holes. Observa

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Cottrell, Geoff. "Multi-messenger astronomy." In Observational Astronomy: A Very Short Introduction, 2nd ed. Oxford University PressOxford, 2023. http://dx.doi.org/10.1093/actrade/9780192849021.003.0006.

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Abstract This chapter highlights the new and different types of astronomical messengers, neutrinos and gravitational waves. These messengers can be detected in regions of the Universe that are electromagnetically hidden from view, and so are highly informative. Neutrinos are produced in massive numbers in the core of the Sun and stars, and also in the most violent events in the Universe, such as in supernovae and the accretion discs around black holes and AGN. Because they interact so weakly with normal matter, neutrinos are difficult to detect, and astronomers look for the rare interactions w

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Criss, Robert E., and Anne M. Hofmeister. "How spin down and radioactive decay drive rocky planet evolution." In In the Footsteps of Warren B. Hamilton: New Ideas in Earth Science. Geological Society of America, 2022. http://dx.doi.org/10.1130/2021.2553(19).

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ABSTRACT Most differences in the gross surface morphologies, tectonic styles, overall geologic histories, and atmospheres of the rocky bodies in the solar system can be explained by contributions and dissipation of gravitational and radiogenic energy over geologic time. These two energy sources are large and measurable and can be extrapolated back in time. Accretion was likely cold, and directly converted gravitational potential energy into axial spin, a prominent feature of planets that is otherwise unexplained. Impact heating was mostly limited to planetary surfaces in the final stages of ac

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Streszczenia konferencji na temat "Accretion; gravitational"

Poggiani, Rosa. "Gravitational Waves from Accreting Sources." In Accretion Processes in Cosmic Sources – II. Sissa Medialab, 2020. http://dx.doi.org/10.22323/1.342.0058.

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Nagar, Alessandro. "Gravitational waves from oscillating accretion tori." In ALBERT EINSTEIN CENTURY INTERNATIONAL CONFERENCE. AIP, 2006. http://dx.doi.org/10.1063/1.2399645.

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Isern, J. "White dwarf merging and the emission of gravitational waves." In INTERACTING BINARIES: Accretion, Evolution, and Outcomes. AIP, 2005. http://dx.doi.org/10.1063/1.2130268.

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Nagar, Alessandro. "Gravitational wave emission from matter accretion onto a Schwarzschild black hole." In GENERAL RELATIVITY AND GRAVITATIONAL PHYSICS: 16th SIGRAV Conference on General Relativity and Gravitational Physics. AIP, 2005. http://dx.doi.org/10.1063/1.1891558.

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Kalogera, Vassiliki. "Compact binary mergers and accretion-induced collapse: Event rates." In Third edoardo amaldi conference on gravitational waves. AIP, 2000. http://dx.doi.org/10.1063/1.1291838.

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Becerra Bayona, Laura Marcela, Carlo Luciano Bianco, Maxime Enderli, et al. "Hypercritical accretion, induced gravitational collapse and binary driven Hypernovae." In Swift: 10 Years of Discovery. Sissa Medialab, 2015. http://dx.doi.org/10.22323/1.233.0171.

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McClintock, Jeffrey E. "Probing strong gravitational fields in X-ray novae." In Accretion processes in astrophysical systems: Some like it hot! - eigth astrophysics conference. AIP, 1998. http://dx.doi.org/10.1063/1.55909.

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Tavleev, A., K. Malanchev, and G. Lipunova. "Vertical structure of accretion discs in LMXB." In The multi-messenger astronomy: gamma-ray bursts, search for electromagnetic counterparts to neutrino events and gravitational waves. Sneg, 2019. http://dx.doi.org/10.26119/sao.2019.1.35553.

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Greyber, Howard D. "Accretion, gravitational collapse and AGN central engine formation in a uniform primordial magnetic field." In Accretion processes in astrophysical systems: Some like it hot! - eigth astrophysics conference. AIP, 1998. http://dx.doi.org/10.1063/1.55946.

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Markozov, I. D. "Modeling pulse profiles in X-Ray pulsars with accretion column." In Всероссийская с международным участием научная конференция студентов и молодых ученых, посвященная памяти Полины Евгеньевны Захаровой «Астрономия и исследование космического пространства». Ural University Press, 2021. http://dx.doi.org/10.15826/b978-5-7996-3229-8.09.

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The pulse profiles of the radiation coming from X-ray pulsars with an accretion column were modeled. Gravitational lensing and redshift in the Schwarzschild metric, as well as the reflection of X-Ray photons from the surface of a neutron star, were taken into account. On the basis of the obtained pulse profiles an analysis of possible errors in the measurements of the luminosities of X-ray pulsars associated with the inability of the observer to correctly take into account the anisotropy in the radiation emerging from the neutron star, as well as the angles between the pulsar’s rotation axis,

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