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Journal articles on the topic 'Mass Accretion Rate'

Author: Grafiati

Published: 5 June 2025

Last updated: 1 August 2025

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1

Fiorellino, E., S. Park, Á. Kóspál, and P. Ábrahám. "The Accretion Process in the DQ Tau Binary System." Astrophysical Journal 928, no. 1 (2022): 81. http://dx.doi.org/10.3847/1538-4357/ac4790.

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Abstract Mass accretion from the circumstellar disk onto the protostar is a fundamental process during star formation. Measuring the mass accretion rate is particularly challenging for stars belonging to binary systems, because it is often difficult to discriminate which component is accreting. DQ Tau is an almost equal-mass spectroscopic binary system where the components orbit each other every 15.8 days. The system is known to display pulsed accretion, i.e., the periodic modulation of the accretion by the components on eccentric orbit. We present multi-epoch ESO/Very Large Telescope X-Shoote

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Kazanas, Demosthenes. "MHD Accretion Disk Winds: The Key to AGN Phenomenology?" Galaxies 7, no. 1 (2019): 13. http://dx.doi.org/10.3390/galaxies7010013.

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Accretion disks are the structures which mediate the conversion of the kinetic energy of plasma accreting onto a compact object (assumed here to be a black hole) into the observed radiation, in the process of removing the plasma’s angular momentum so that it can accrete onto the black hole. There has been mounting evidence that these structures are accompanied by winds whose extent spans a large number of decades in radius. Most importantly, it was found that in order to satisfy the winds’ observational constraints, their mass flux must increase with the distance from the accreting object; the

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Haemmerlé, L., R. S. Klessen, L. Mayer, and L. Zwick. "Maximum accretion rate of supermassive stars." Astronomy & Astrophysics 652 (August 2021): L7. http://dx.doi.org/10.1051/0004-6361/202141376.

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Context. The formation of the most massive quasars observed at high redshifts requires extreme inflows of gas down to the length scales of the central compact object. Aims. Here we estimate the maximum inflow rate allowed by gravity down to the surface of supermassive stars, the possible progenitors of these supermassive black holes. Methods. We use the continuity equation and the assumption of spherical symmetry and free fall to derive the maximum allowed inflow rates for various density profiles. We apply our approach to the mass–radius relation of rapidly accreting supermassive stars to est

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Park, Myeong-Gu. "MASS ACCRETION RATE OF ROTATING VISCOUS ACCRETION FLOW." Astrophysical Journal 706, no. 1 (2009): 637–43. http://dx.doi.org/10.1088/0004-637x/706/1/637.

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Bergez-Casalou, C., B. Bitsch, A. Pierens, A. Crida, and S. N. Raymond. "Influence of planetary gas accretion on the shape and depth of gaps in protoplanetary discs." Astronomy & Astrophysics 643 (November 2020): A133. http://dx.doi.org/10.1051/0004-6361/202038304.

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It is widely known that giant planets have the capacity to open deep gaps in their natal gaseous protoplanetary discs. It is unclear, however, how gas accretion onto growing planets influences the shape and depth of their growing gaps. We performed isothermal hydrodynamical simulations with the Fargo-2D1D code, which assumes planets accreting gas within full discs that range from 0.1 to 260 AU. The gas accretion routine uses a sink cell approach, in which different accretion rates are used to cope with the broad range of gas accretion rates cited in the literature. We find that the planetary g

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Hashimoto, Jun, and Yuhiko Aoyama. "Analyses of Multiple Balmer Emission Lines from Accreting Brown Dwarfs and Very Low Mass Stars." Astronomical Journal 169, no. 2 (2025): 93. https://doi.org/10.3847/1538-3881/ad957e.

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Abstract A planetary growth rate, i.e., the mass accretion rate, is a fundamental parameter in planet formation, as it determines a planet's final mass. Planetary mass accretion rates have been estimated using hydrogen lines, based on the models originally developed for accreting stars, known as the accretion flow model. Recently, Aoyama et al. introduced the accretion shock model as an alternative mechanism for hydrogen line emission. However, it remains unclear which model is more appropriate for accreting planets and substellar objects. To address this, we applied both models to archival da

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Herczeg 沈, Gregory J. 雷歌, Yuguang 昱光 Chen 陈, Jean-Francois Donati, et al. "Twenty-five Years of Accretion onto the Classical T Tauri Star TW Hya." Astrophysical Journal 956, no. 2 (2023): 102. http://dx.doi.org/10.3847/1538-4357/acf468.

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Abstract Accretion plays a central role in the physics that governs the evolution and dispersal of protoplanetary disks. The primary goal of this paper is to analyze the stability over time of the mass accretion rate onto TW Hya, the nearest accreting solar-mass young star. We measure veiling across the optical spectrum in 1169 archival high-resolution spectra of TW Hya, obtained from 1998–2022. The veiling is then converted to accretion rate using 26 flux-calibrated spectra that cover the Balmer jump. The accretion rate measured from the excess continuum has an average of 2.51 × 10−9 M ⊙ yr−1

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Maeda, Natsuho, Keiji Ohtsuki, Takayuki Tanigawa, Masahiro N. Machida, and Ryo Suetsugu. "Delivery of Gas onto the Circumplanetary Disk of Giant Planets: Planetary-mass Dependence of the Source Region of Accreting Gas and Mass Accretion Rate." Astrophysical Journal 935, no. 1 (2022): 56. http://dx.doi.org/10.3847/1538-4357/ac7ddf.

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Abstract Gas accretion onto the circumplanetary disks and the source region of accreting gas are important to reveal dust accretion that leads to satellite formation around giant planets. We performed local three-dimensional high-resolution hydrodynamic simulations of an isothermal and inviscid gas flow around a planet to investigate the planetary-mass dependence of the gas accretion bandwidth and gas accretion rate onto circumplanetary disks. We examined cases with various planetary masses corresponding to M p = 0.05–1M Jup at 5.2 au, where M Jup is the current Jovian mass. We found that the

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Bosch-Ramon, V. "3D hydrodynamical simulations of the impact of mechanical feedback on accretion in supersonic stellar-mass black holes." Astronomy & Astrophysics 660 (March 30, 2022): A5. http://dx.doi.org/10.1051/0004-6361/202142821.

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Context. Isolated stellar-mass black holes accrete gas from their surroundings, often at supersonic speeds, and can form outflows that may influence the accreted gas. The latter process, known as mechanical feedback, can significantly affect the accretion rate. Aims. We use hydrodynamical simulations to assess the impact of mechanical feedback on the accretion rate when the black hole moves supersonically through a uniform medium. Methods. We carried out three-dimensional (3D) hydrodynamical simulations of outflows fueled by accretion that interact with a uniform medium, probing scales equival

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Naddaf, Mohammad-Hassan, Bożena Czerny, and Michal Zajaček. "The Wind Dynamics of Super-Eddington Sources in FRADO." Dynamics 2, no. 3 (2022): 295–305. http://dx.doi.org/10.3390/dynamics2030015.

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We perform non-hydrodynamical 2.5D simulations to study the dynamics of material above accretion disk based on the disk radiation pressure acting on dust. We assume a super-accreting underlying disk with the accretion rate of 10 times the Eddington rate with central black hole mass ranging from 107 up to 109M⊙. Such high accretion rates are characteristic for extreme sources. We show that for high accretors the radiatively dust-driving mechanism based on the FRADO model always leads to a massive outflow from the disk surface, and the failed wind develops only at larger radii. The outflow rate

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Fiorellino, Eleonora, Carlo F. Manara, Brunella Nisini, et al. "KMOS study of the mass accretion rate from Class I to Class II in NGC 1333." Astronomy & Astrophysics 650 (June 2021): A43. http://dx.doi.org/10.1051/0004-6361/202039264.

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Context. The mass accretion rate (Ṁacc) is the fundamental parameter to understand the process of mass assembly that results in the formation of a low-mass star. This parameter has been largely studied in Classical T Tauri stars in star-forming regions with ages of ∼1 − 10 Myr. However, little is known about the accretion properties of young stellar objects (YSOs) in younger regions and early stages of star formation, such as in the Class 0/I phases. Aims. We present new near-infrared spectra of 17 Class I/Flat and 35 Class II sources located in the young (< 1 Myr) NGC 1333 cluster, acquire

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KINASIEWICZ, BOGUSZ, PATRYK MACH, and EDWARD MALEC. "SELFGRAVITATION IN A GENERAL-RELATIVISTIC ACCRETION OF STEADY FLUIDS." International Journal of Geometric Methods in Modern Physics 04, no. 01 (2007): 197–208. http://dx.doi.org/10.1142/s0219887807001953.

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The selfgravity of an infalling gas can alter significantly the accretion of gases. In the case of spherically symmetric steady flows of polytropic perfect fluids the mass accretion rate achieves maximal value when the mass of the fluid is 1/3 of the total mass. There are two weakly accreting regimes, one over-abundant and the other poor in fluid content. The analysis within the newtonian gravity suggests that selfgravitating fluids can be unstable, in contrast to the accretion of test fluids.

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Zhang, Zhengyang, Chengyuan Wu, Amar Aryan, Shuai Zha, Dongdong Liu, and Bo Wang. "He-accreting Oxygen–Neon White Dwarfs and Accretion-induced Collapse Events." Astrophysical Journal 975, no. 2 (2024): 186. http://dx.doi.org/10.3847/1538-4357/ad7e13.

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Abstract It has been widely accepted that mass-accreting white dwarfs (WDs) are the progenitors of Type Ia supernovae (SNe) or electron-capture supernovae. Previous work has shown that the accretion rate could affect the elemental abundance on the outer layers of CO WDs, and therefore affect the observational characteristics after they exploded as SNe Ia. However, it has not been well studied how elemental abundance changes on the outer layers of He-accreting ONe WDs as they approach the Chandrasekhar mass limit. In this paper, we investigated the evolution of He-accreting ONe WDs with MESA. W

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Seifina, Elena, Alexandre Chekhtman, and Lev Titarchuk. "NGC 4051: Black hole mass and photon index-mass accretion rate correlation." Astronomy & Astrophysics 613 (May 2018): A48. http://dx.doi.org/10.1051/0004-6361/201732235.

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We present a discovery of the correlation between the X-ray spectral (photon) index and mass accretion rate observed in an active galactic nucleus, NGC 4051. We analyzed spectral transition episodes observed in NGC 4051 using XMM-Newton, Suzaku and RXTE. We applied a scaling technique for a black hole (BH) mass evaluation which uses a correlation between the photon index and normalization of the seed (disk) component, which is proportional to a mass accretion rate. We developed an analytical model that shows the spectral (photon) index of the BH emergent spectrum undergoes an evolution from lo

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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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Betti, S. K., K. B. Follette, K. Ward-Duong, et al. "Near-infrared Accretion Signatures from the Circumbinary Planetary-mass Companion Delorme 1 (AB)b*." Astrophysical Journal Letters 935, no. 1 (2022): L18. http://dx.doi.org/10.3847/2041-8213/ac85ef.

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Abstract Accretion signatures from bound brown dwarf and protoplanetary companions provide evidence for ongoing planet formation, and accreting substellar objects have enabled new avenues to study the astrophysical mechanisms controlling the formation and accretion processes. Delorme 1 (AB)b, a ∼30–45 Myr circumbinary planetary-mass companion, was recently discovered to exhibit strong Hα emission. This suggests ongoing accretion from a circumplanetary disk, somewhat surprising given canonical gas disk dispersal timescales of 5–10 Myr. Here, we present the first NIR detection of accretion from

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Ikhsanov, N. R., and N. G. Beskrovnaya. "Deceleration of the disk by the accreting magnetized star in the corotation approximation." Publications of the Pulkovo Observatory 229 (August 2023): 1–5. http://dx.doi.org/10.31725/0367-7966-2023-229-3.

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We study the process of interaction of an accretion disk with the dipole magnetic field of an accreting star within the corotation approximation. Using dynamical accretion picture we calculate the radius at which the gaseous pressure in the disk is balanced by the pressure of the dipole magnetic field of the accreting star and simultaneously the mass accretion rate in the disk is balanced by the rate of plasma diffusion into the stellar magnetic field. We show that the magnetospheric radius calculated under these conditions in a wide range of parameters is significantly smaller than the canoni

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Akil, Ali, and Qianhang Ding. "A dark matter probe in accreting pulsar-black hole binaries." Journal of Cosmology and Astroparticle Physics 2023, no. 09 (2023): 011. http://dx.doi.org/10.1088/1475-7516/2023/09/011.

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Abstract The accretion of dark matter (DM) into astrophysical black holes slowly increases their mass. The rate of this mass accretion depends on the DM model and the model parameters. If this mass accretion effect can be measured accurately enough, it is possible to rule out some DM models, and, with the sufficient technology and the help of other DM constraints, possibly confirm one model. We propose a DM probe based on accreting pulsar-black hole binaries, which provide a high-precision measurement on binary orbital phase shifts induced by DM accretion into black holes, and can help rule ou

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Yusupova, Rosaliya M., Ramis Kh Karimov, Ramil N. Izmailov, and Kamal K. Nandi. "Accretion Flow onto Ellis–Bronnikov Wormhole." Universe 7, no. 6 (2021): 177. http://dx.doi.org/10.3390/universe7060177.

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Study of accretion onto wormholes is rather rare compared to that onto black holes. In this paper, we consider accretion flow of cosmological dark energy modeled by barotropic fluid onto the celebrated Ellis–Bronnikov wormhole (EBWH) built by Einstein minimally coupled scalar field ϕ, violating the null energy condition. The accreting fluid is assumed to be phantom, quintessence, dust and stiff matter. We begin by first pointing out a mathematical novelty showing how the EBWH can lead to the Schwarzschild black hole under a complex Wick rotation. Then, we analyze the profiles of fluid radial v

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Fiorellino, Eleonora, Łukasz Tychoniec, Fernando Cruz-Sáenz de Miera, et al. "The Mass Accretion Rate and Stellar Properties in Class I Protostars." Astrophysical Journal 944, no. 2 (2023): 135. http://dx.doi.org/10.3847/1538-4357/aca320.

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Abstract Stars collect most of their mass during the protostellar stage, yet the accretion luminosity and stellar parameters, which are needed to compute the mass accretion rate, are poorly constrained for the youngest sources. The aim of this work is to fill this gap, computing the stellar properties and the accretion rates for a large sample of Class I protostars located in nearby (<500 pc) star-forming regions and analyzing their interplay. We used a self-consistent method to provide accretion and stellar parameters by modeling the spectral energy distribution and using veiling informati

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Marleau, Gabriel-Dominique, Yuhiko Aoyama, Jun Hashimoto, and Yifan Zhou. "Revisiting the Helium and Hydrogen Accretion Indicators at TWA 27B: Weak Mass Flow at Near-freefall Velocity." Astrophysical Journal 964, no. 1 (2024): 70. http://dx.doi.org/10.3847/1538-4357/ad1ee9.

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Abstract TWA 27B (2M1207b) is the first directly imaged planetary-mass (M p ≈ 5 M J) companion and was observed at 0.9–5.3 μm with JWST/NIRSpec. To understand the accretion properties of TWA 27B, we search for continuum-subtracted near-infrared helium and hydrogen emission lines and measure their widths and luminosities. We detect the He i triplet at 4.3σ and all Paschen-series lines covered by NIRSpec (Paα, Paβ, Paγ, Paδ) at 4σ–5σ. The three brightest Brackett-series lines (Brα, Brβ, Brγ) as well as Pfγ and Pfδ are tentative detections at 2σ–3σ. We provide upper limits on the other hydroge

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KAUFMAN BERNADÓ, M. M., and M. MASSI. "JET FORMATION IN MICROQUASARS AND ACTIVE GALACTIC NUCLEI: MAGNETIC FIELD LIMITS." International Journal of Modern Physics D 17, no. 10 (2008): 1931–37. http://dx.doi.org/10.1142/s0218271808013595.

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We introduce the use of a well-known parameter, the Alfvén Radius, R A , as a new tool to discern whether an X-ray binary system may undergo a microquasar phase, i.e. ejecting relativistic particles orthogonal to the accretion disk. We study what we call the basic condition, R A /R* = 1 in its dependency on the magnetic field strength and the mass accretion rate. With this basic condition we establish under which combination of parameters any class of accreting neutron stars could become a microquasar instead of confining disk-material down to the magnetic poles and creating the two emitting c

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Essex, Christopher, Shantanu Basu, Janett Prehl, and Karl Heinz Hoffmann. "A multiple power-law distribution for initial mass functions." Monthly Notices of the Royal Astronomical Society 494, no. 2 (2020): 1579–86. http://dx.doi.org/10.1093/mnras/staa755.

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ABSTRACT We introduce a new multi-power-law distribution for the initial mass function (IMF) to explore its potential properties. It follows on prior work that introduced mechanisms accounting for mass accretion in star formation, developed within the framework of general evolution equations for the mass distribution of accreting and non-accreting (proto)stars. This paper uses the same fundamental framework to demonstrate that the interplay between a mass-dependent and a time-dependent step-like dropout rate from accretion leads to IMFs that exhibit multiple power laws for an exponential mass

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Alcalá, J. M., C. F. Manara, K. France, et al. "HST spectra reveal accretion in MY Lupi." Astronomy & Astrophysics 629 (September 2019): A108. http://dx.doi.org/10.1051/0004-6361/201935657.

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The mass accretion rate is a crucial parameter for the study of the evolution of accretion discs around young low-mass stellar and substellar objects (YSOs). We revisit the case of MY Lup, an object where VLT/X-shooter data suggested a negligible mass accretion rate, and show it to be accreting on a level similar to other Class II YSOs in Lupus based on Hubble Space Telescope (HST) observations. In our HST-Cosmic Origins Spectrograph (HST-COS) and -Space Telescope Imaging Spectrograph (HST-STIS) spectra, we find many emission lines, as well as substantial far-ultraviolet (FUV) continuum excess

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Karovska, M., B. Wood, M. Marengo, J. C. Raymond, W. Hack, and E. Guinan. "Accretion Processes in Mira AB." International Astronomical Union Colloquium 194 (2004): 92–94. http://dx.doi.org/10.1017/s0252921100152042.

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AbstractThe Mira AB interacting binary provides an ideal laboratory for studying mass loss and accretion processes in systems containing an AGB star and a compact accretor, because its components have been resolved and can be studied individually. We present here results from our long term study of accretion processes in this system. Those include recent HST observations suggesting that the accretion rate onto Mira B is much lower than before, indicating possible disruption of the accretion disk.

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Chakraborty, Sudip, Ajay Ratheesh, Francesco Tombesi, Rodrigo Nemmen, and Srimanta Banerjee. "Universality of coronal properties in accreting black holes across mass and accretion rate." Astronomy & Astrophysics 676 (August 2023): L13. http://dx.doi.org/10.1051/0004-6361/202347181.

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Aims. Through their radio loudness, lack of thermal UV emission from the accretion disk, and power-law dominated spectra, low-luminosity active galactic nuclei (LLAGNs) display similarity with the hard state of stellar-mass black hole X-ray binaries (BHBs). In this work we perform a systematic hard X-ray spectral study of a carefully selected sample of unobscured LLAGNs using archival NuSTAR data to understand the central engine properties in the lower accretion regime. Methods. We analyzed the NuSTAR spectra of a sample of 16 LLAGNs. We modeled the continuum emission with detailed Comptonizat

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Cumming, Andrew. "Magnetic Field Evolution in Accreting White Dwarfs." International Astronomical Union Colloquium 190 (2004): 58–70. http://dx.doi.org/10.1017/s025292110000186x.

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AbstractI discuss the effect of accretion on the magnetic field of an accreting white dwarf. Whereas the magnetic fields of isolated white dwarfs are not expected to change significantly with time, I show that if an accreting white dwarf increases in mass at a rate > 1–5 × 10−10MΘ yr–1, accretion overcomes ohmic diffusion and has a significant effect on the field structure. I discuss the implications of this result for observed systems. In particular, accretion induced field evolution may provide the missing evolutionary link between the strong field, slowly accreting AM Her systems and the

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Marleau, G. D., Y. Aoyama, R. Kuiper та ін. "Accreting protoplanets: Spectral signatures and magnitude of gas and dust extinction at H α". Astronomy & Astrophysics 657 (24 грудня 2021): A38. http://dx.doi.org/10.1051/0004-6361/202037494.

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Context. Accreting planetary-mass objects have been detected at H α, but targeted searches have mainly resulted in non-detections. Accretion tracers in the planetary-mass regime could originate from the shock itself, making them particularly susceptible to extinction by the accreting material. High-resolution (R > 50 000) spectrographs operating at H α should soon enable one to study how the incoming material shapes the line profile. Aims. We calculate how much the gas and dust accreting onto a planet reduce the H α flux from the shock at the planetary surface and how they affect the line s

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Nomura, Mariko, Ken Ohsuga, and Chris Done. "Line-driven disc wind in near-Eddington active galactic nuclei: decrease of mass accretion rate due to powerful outflow." Monthly Notices of the Royal Astronomical Society 494, no. 3 (2020): 3616–26. http://dx.doi.org/10.1093/mnras/staa948.

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ABSTRACT Based on recent X-ray observations, ultrafast outflows from supermassive black holes are expected to have enough energy to dramatically affect their host galaxy but their launch and acceleration mechanisms are not well understood. We perform two-dimensional radiation hydrodynamics simulations of UV line-driven disc winds in order to calculate the mass-loss rates and kinetic power in these models. We develop a new iterative technique that reduces the mass accretion rate through the inner disc in response to the wind mass-loss. This makes the inner disc less UV bright, reducing the wind

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Hachisu, Izumi. "RX J0513.9-6951 and V Sagittae: Accretion Wind Evolution, A Key Evolutionary Process to Type IA Supernovae." International Astronomical Union Colloquium 194 (2004): 106–8. http://dx.doi.org/10.1017/s0252921100152091.

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AbstractA new self-sustained model for long-term light-curve variations of the supersoft X-ray sources RX J0513.9–6951 and V Sge is proposed based on an optically thick wind model of mass-accreting white dwarfs (WDs). When the mass accretion rale to a WD exceeds the critical rate of ~ 1 x 10–1M⊙. yr–1, optically thick strong winds begin to blow from the WD so that a formation of common envelope is avoided. The WD can accrete and burn hydrogen-rich matter on the surface of the WD at the critical rate. The excess matter transferred to the WD above the critical rate is expelled by winds. This is

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Grichener, Aldana, Coral Cohen, and Noam Soker. "Simulating the Negative Jet Feedback Mechanism in Common Envelope Jet Supernovae." Astrophysical Journal 922, no. 1 (2021): 61. http://dx.doi.org/10.3847/1538-4357/ac23dd.

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Abstract We use the stellar evolution code MESA to study the negative jet feedback mechanism in common envelope jet supernovae (CEJSNe), in which a neutron star (NS) launches jets in the envelope of a red supergiant (RSG). We find that the feedback reduces the mass accretion rate to be χ j ≃ 0.04–0.3 times the mass accretion rate without the operation of jets. We mimic the effect of the jets on the RSG envelope by depositing the energy that the jets carry into the envelope zones outside the NS orbit. The energy deposition inflates the envelope, therefore reducing the density in the NS vicinity

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Brouwers, M. G., C. W. Ormel, A. Bonsor, and A. Vazan. "How planets grow by pebble accretion." Astronomy & Astrophysics 653 (September 2021): A103. http://dx.doi.org/10.1051/0004-6361/202140476.

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Context. In the theory of pebble accretion, planets form by the subsequent accretion of solids (micron-sized dust and larger pebbles) and gas. The amount of nebular gas that a planet can bind is limited by its cooling rate, which is set by the opacity of its envelope. Accreting dust and pebbles contribute to the envelope opacity and, thus, influence the outcome of planet formation. Aims. Our aim is to model the size evolution and opacity contribution of solids inside planetary envelopes. We then use the resultant opacity relations to study emergent trends in planet formation. Methods. We desig

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Tognelli, Emanuele, Pier Giorgio Prada Moroni, Scilla Degl’Innocenti, Maurizio Salaris, and Santi Cassisi. "Protostellar accretion in low mass metal poor stars and the cosmological lithium problem." Astronomy & Astrophysics 638 (June 2020): A81. http://dx.doi.org/10.1051/0004-6361/201936723.

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Context. The cosmological lithium problem, that is, the discrepancy between the lithium abundance predicted by the Big Bang nucleosynthesis and the one observed for the stars of the “Spite plateau”, is one of the long standing problems of modern astrophysics. Recent hints for a possible solution involve lithium burning induced by protostellar mass accretion on Spite plateau stars. However, to date, most of the protostellar and pre-main sequence stellar models that take mass accretion into account have been computed at solar metallicity, and a detailed analysis on the impact of protostellar acc

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Hadrava, Petr, and Jan Čechura. "Accretion of stellar winds in high-mass X-ray binaries." Proceedings of the International Astronomical Union 8, S290 (2012): 219–20. http://dx.doi.org/10.1017/s1743921312019709.

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AbstractOur analysis of optical spectroscopy of high-mass X-ray binaries like Cyg X-1 confirms that most of the Balmer-lines emission anticorrelated with the X-ray flux originates from the circumstellar matter between the donor star and the accreting compact component. In order to study its structure and variability and the consequent accretion rate we have developed a 3-D numerical model based on radiation hydrodynamics of the supergiant stellar wind. The results show a non-stationary BHL-accretion on the compact component.

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Hillman, Yael, and Amit Kashi. "Simulations of multiple nova eruptions induced by wind accretion in symbiotic systems." Monthly Notices of the Royal Astronomical Society 501, no. 1 (2020): 201–9. http://dx.doi.org/10.1093/mnras/staa3600.

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ABSTRACT We use a combined binary evolution code including dynamical effects to study nova eruptions in a symbiotic system. Following the evolution, over ∼105 yr, of multiple consecutive nova eruptions on the surface of a $1.25\hbox{-}\rm {M_\odot }$ white dwarf (WD) accretor, we present a comparison between simulations of two types of systems. The first is the common, well-known, cataclysmic variable (CV) system in which a main-sequence donor star transfers mass to its WD companion via Roche lobe overflow. The second is a detached, widely separated, symbiotic system in which an asymptotic gia

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Maithil, Jaya, Michael S. Brotherton, Bin Luo, et al. "X-ray properties of reverberation-mapped AGNs with super-Eddington accreting massive black holes." Proceedings of the International Astronomical Union 15, S356 (2019): 143. http://dx.doi.org/10.1017/s1743921320002756.

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AbstractActive Galactic Nuclei (AGN) exhibit multi-wavelength properties that are representative of the underlying physical processes taking place in the vicinity of the accreting supermassive black hole. The black hole mass and the accretion rate are fundamental for understanding the growth of black holes, their evolution, and the impact on the host galaxies. Recent results on reverberation-mapped AGNs show that the highest accretion rate objects have systematic shorter time-lags. These super-Eddington accreting massive black holes (SEAMBHs) show BLR size 3-8 times smaller than predicted by t

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Speicher, J., D. R. Ballantyne, and P. C. Fragile. "Examining the Relationship between the Persistent Emission and the Accretion Rate during a Type I X-Ray Burst." Astrophysical Journal 976, no. 1 (2024): 44. http://dx.doi.org/10.3847/1538-4357/ad863d.

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Abstract The accretion flow onto a neutron star will be impacted by irradiation from a type I X-ray burst. The burst radiation exerts Poynting–Robertson (PR) drag on the accretion disk, leading to an enhanced mass accretion rate. Observations of X-ray bursts often find evidence that the normalization of the disk-generated persistent emission (commonly denoted by the factor f a ) increases during a burst, and changes in f a have been used to infer the evolution of the mass accretion rate due to PR drag. Here, we examine this proposed relationship between f a and mass accretion rate enhancement

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Laune, JT, Rixin 日新 Li 李, and Dong Lai. "Migration of Accreting Planets and Black Holes in Disks." Astrophysical Journal 975, no. 2 (2024): 296. http://dx.doi.org/10.3847/1538-4357/ad7117.

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Abstract Nascent planets are thought to lose angular momentum (AM) to the gaseous protoplanetary disk via gravitational interactions, leading to inward migration. A similar migration process also applies to stellar-mass black holes (BHs) embedded in the disks of active galactic nuclei. However, AM exchange via accretion onto the planet/BH may strongly influence the migration torque. In this study, we perform 2D global hydrodynamic simulations of an accreting planet/BH embedded in a disk, where AM exchange between the planet/BH and disk via gravity, accretion, pressure, and viscosity are consid

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Liu, Helei, Yong Gao, Zhaosheng Li, et al. "EOS-dependent millihertz quasi-periodic oscillation in low-mass X-ray binary." Monthly Notices of the Royal Astronomical Society 525, no. 2 (2023): 2054–68. http://dx.doi.org/10.1093/mnras/stad2424.

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ABSTRACT We studied the frequency and critical mass accretion rate of millihertz quasi-periodic oscillations (mHz QPOs) using a one-zone X-ray burst model. The surface gravity is specified by two kinds of equation of states: neutron star (NS) and strange star (SS). The base flux, Qb, is set in the range of 0–2 MeV nucleon−1. It is found that the frequency of mHz QPO is positively correlated to the surface gravity but negatively to the base heating. The helium mass fraction has a significant influence on the oscillation frequency and luminosity. The observed 7–9 mHz QPOs can be either explained

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Kato, Mariko, Hideyuki Saio, and Izumi Hachisu. "A light curve model of V2491 Cyg: Classical nova outburst on a cool and massive white dwarf." Publications of the Astronomical Society of Japan 73, no. 4 (2021): 1137–51. http://dx.doi.org/10.1093/pasj/psab064.

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Abstract The classical nova V2491 Cyg was once suggested to be a recurrent nova. We have broadly reproduced the light curve of V2491 Cyg by a nova outburst model on a cold 1.36 M⊙ white dwarf (WD), which strongly suggests that V2491 Cyg is a classical nova outbursting on a cold very massive WD rather than a recurrent nova outbursting on a warmer WD like the recurrent nova RS Oph. In the long-term evolution of a cataclysmic binary, an accreting WD has settled to a thermal equilibrium state with the balance of gravitational energy release and neutrino loss. The central temperature of the WD is u

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Ginzburg, Sivan, and Eugene Chiang. "Heavy-metal Jupiters by major mergers: metallicity versus mass for giant planets." Monthly Notices of the Royal Astronomical Society 498, no. 1 (2020): 680–88. http://dx.doi.org/10.1093/mnras/staa2500.

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ABSTRACT Some Jupiter-mass exoplanets contain ${\sim}100\, {\rm M}_{\hbox{$\oplus $}}$ of metals, well above the ${\sim}10\, {\rm M}_{\hbox{$\oplus $}}$ typically needed in a solid core to trigger giant planet formation by runaway gas accretion. We demonstrate that such ‘heavy-metal Jupiters’ can result from planetary mergers near ∼10 au. Multiple cores accreting gas at runaway rates gravitationally perturb one another on to crossing orbits such that the average merger rate equals the gas accretion rate. Concurrent mergers and gas accretion implies the core mass scales with the total planet ma

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Sneha, Dey, and Ghorai A. "A Comprehensive Study of Mass Accretion and Atmospheric Effect of Raindrop." Indian Journal of Advanced Physics (IJAP) 1, no. 3 (2022): 5–9. https://doi.org/10.54105/ijap.C1018.041322.

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The mass accretion of a raindrop in different layers of the atmosphere is not dealt with so far. A comprehensive brief study of the motion of raindrops through the atmosphere (i) without mass accretion, (ii) with mass accretion and (iii) finally pressure variation in the atmosphere with altitude using Bernoulli’s equation is illustrated. Acquirement of mass from moist air is mass accretion and mass accretion during the motion of raindrop through resistive medium holds an arbitrary power-law equation. Bernoulli’s equation when applied to it, the generalized first-order differential

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Plunkett, Cailin, Katherine B. Follette, Gabriel-Dominique Marleau та Eric L. Nielsen. "Occurrence Rates of Accreting Companions from a New Method for Computing Emission-line Survey Sensitivity: Application to the Hα Giant Accreting Protoplanet Survey". Astronomical Journal 169, № 5 (2025): 262. https://doi.org/10.3847/1538-3881/adc09d.

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Abstract A key scientific goal of exoplanet surveys is to characterize the underlying population of planets in the local galaxy. In particular, the properties of accreting protoplanets can inform the rates and physical processes of planet formation. We develop a novel method to compute sensitivity to protoplanets in emission-line direct-imaging surveys, enabling estimates of protoplanet population properties under various planetary accretion and formation theories. In this work, we specialize to the case of Hα and investigate three formation models governing the planetary-mass-to-mass-accretio

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Fiorellino, Eleonora, Gabriella Zsidi, Ágnes Kóspál, et al. "Accretion and Extinction Variations in the Low-mass Pre-main-sequence Binary System WX Cha*." Astrophysical Journal 938, no. 2 (2022): 93. http://dx.doi.org/10.3847/1538-4357/ac912d.

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Abstract Light curves of young star systems show photometric variability due to different kinematic and physical processes. One of the main contributors to the photometric variability is the changing mass accretion rate, which regulates the interplay between the forming young star and the protoplanetary disk. We collected high-resolution spectroscopy in eight different epochs, as well as ground-based and space-borne multiepoch optical and infrared photometry of WX Cha, an M0 binary system, with an almost edge-on disk (i = 87°) in the Chamaeleon I star-forming region. Spectroscopic observations

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Xie, Fu-Guo, Ramesh Narayan, and Feng Yuan. "Observational Constraints on Direct Electron Heating in the Hot Accretion Flows in Sgr A* and M87*." Astrophysical Journal 942, no. 1 (2022): 20. http://dx.doi.org/10.3847/1538-4357/aca534.

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Abstract An important parameter in the theory of hot accretion flows around black holes is δ, which describes the fraction of “viscously” dissipated energy in the accretion flow that goes directly into heating electrons. For a given mass accretion rate, the radiative efficiency of a hot accretion flow is determined by δ. Unfortunately, the value of δ is hard to determine from first principles. The recent Event Horizon Telescope Collaboration (EHTC) results on M87* and Sgr A* provide us with a different way of constraining δ. By combining the mass accretion rates in M87* and Sgr A* estimated by

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Park, Myeong-Gu, and Du-Hwan Han. "Hot Accretion onto Black Holes with Outflow." EPJ Web of Conferences 168 (2018): 04005. http://dx.doi.org/10.1051/epjconf/201816804005.

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Classic Bondi accretion flow can be generalized to rotating viscous accretion flow. Study of hot accretion flow onto black holes show that its physical charateristics change from Bondi-like for small gas angular momentum to disk-like for Keperian gas angular momentum. Especially, the mass accretion rate divided by the Bondi accretion rate is proportional to the viscosity parameter alpha and inversely proportional to the gas angular momentum divided by the Keplerian angular momentum at the Bondi radius for gas angular momentum comparable to the Keplerian value. The possible presence of outflow

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Kato, Mariko, Hideyuki Saio, and Izumi Hachisu. "Growth Rate of White Dwarf Mass in Binaries." International Astronomical Union Colloquium 114 (1989): 507–10. http://dx.doi.org/10.1017/s0252921100100156.

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AbstractThe growth rate of a white dwarf which accretes hydrogen-rich or helium matter is studied. If the accretion rate is relatively small, unstable shell flash occurs and during which the envelope mass is lost. We have followed the evolutions of shell flashes by steady state approach with wind mass loss solutions to determined the mass lost from the system for wide range of binary parameters. The time-dependent models are also calculated in some cases. The mass loss due to the Roche lobe overflow are taken into account. This results seriously affects the existing scenarios on the origin of

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Fiorellino, Eleonora, Łukasz Tychoniec, Carlo F. Manara, et al. "The Relation between the Mass Accretion Rate and the Disk Mass in Class I Protostars." Astrophysical Journal Letters 937, no. 1 (2022): L9. http://dx.doi.org/10.3847/2041-8213/ac8fee.

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Abstract Evidence of a relation between the mass accretion rate and the disk mass is established for young, Class II pre-main-sequence stars. This observational result opened an avenue to test theoretical models and constrain the initial conditions of disk formation, fundamental in the understanding of the emergence of planetary systems. However, it is becoming clear that planet formation starts even before the Class II stage, in disks around Class 0 and I protostars. We show for the first time evidence for a correlation between the mass accretion rate and the disk mass for a large sample of C

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Singh, Akshay, Damien Bégué, and Asaf Pe’er. "Radiative Cooling Changes the Dynamics of Magnetically Arrested Disks." Astrophysical Journal Letters 981, no. 1 (2025): L11. https://doi.org/10.3847/2041-8213/adb749.

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Abstract We study magnetically arrested disks (MADs) around rotating black holes (BHs) under the influence of radiative cooling. We introduce a critical value of the mass accretion rate M ̇ crit for which the cooling by the synchrotron process efficiently radiates the thermal energy of the disk. We find M ̇ crit ≈ 1 0 − 5.5 M ̇ Edd , where M ̇ Edd is the Eddington mass accretion rate. The normalization constant depends on the saturated magnetic flux and on the ratio of electron to proton temperatures, but not on the BH mass. We verify our analytical estimate using a suite of general relativist

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Lei, Y. J., H. T. Zhang, Y. Q. Dong, and H. L. Yuan. "The type I X-ray bursts of 4U 1735–44." Proceedings of the International Astronomical Union 8, S290 (2012): 251–52. http://dx.doi.org/10.1017/s1743921312019862.

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AbstractWith RXTE data ranging from 1997 August to 1998 May, we detected 8 type I X-ray bursts from the atoll source 4U 1735–44. The bursts are present at all the branches, and most occur at an inferred low mass accretion rate. We find no correlation between the peak flux of the bursts and the mass accretion rate. The results are different from that of 4U 1728-34, whose bursts' peak flux are anti-correlated with the mass accretion rate.

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