Zobrazeno 1 - 10
of 244
pro vyhledávání: '"Hameury, J."'
Publikováno v:
A&A 664, A7 (2022)
Some intermediate polars show outbursts that are much shorter than those observed in normal dwarf novae, and whose origin has remained unelucidated for a long time. We examine here the case of V1223 Sgr, an intermediate polar that showed a short outb
Externí odkaz:
http://arxiv.org/abs/2205.11227
Autor:
Sandoval, L. E. Rivera, Heinke, C. O., Hameury, J. M., Cavecchi, Y., Vanmunster, T., Tordai, T., Romanov, F.
ASASSN-21au is an ultracompact accreting white dwarf binary (AM CVn) with a period of approx. 58 min. Using multiwavelength observations of the system, we discovered a dichotomy in the behavior of outbursts in AM CVns. The binary showed an initial br
Externí odkaz:
http://arxiv.org/abs/2107.11006
Autor:
Hameury, J. -M., Lasota, J. -P.
Publikováno v:
A&A 650, A114 (2021)
The disc instability model accounts well for most of the observed properties of dwarf novae and soft X-ray transients, but the rebrightenings, reflares, and echoes occurring at the end of outbursts or shortly after in WZ Sge stars or soft X-ray trans
Externí odkaz:
http://arxiv.org/abs/2104.02952
Publikováno v:
A&A 637, A88 (2020)
The determination of the size and geometry of the broad line region (BLR) in active galactic nuclei is one of the major ingredients for determining the mass of the accreting black hole. This can be done by determining the delay between the optical co
Externí odkaz:
http://arxiv.org/abs/2004.03957
Publikováno v:
A&A 636, A1 (2020)
Context. Although the disc instability model is widely accepted as the explanation for dwarf nova outbursts, it is still necessary to confront its predictions to observations because much of the constraints on angular momentum transport in accretion
Externí odkaz:
http://arxiv.org/abs/2003.03056
Publikováno v:
A&A 632, A40 (2019)
The observed signatures of winds from X-ray binaries are broadly consistent with thermal winds, driven by X-ray irradiation of the outer accretion disc. Thermal winds produce mass outflow rates that can exceed the accretion rate in the disc. We study
Externí odkaz:
http://arxiv.org/abs/1909.13601
Publikováno v:
MNRAS 481 (2018), 5422 - 5435
Using the disc instability model for dwarf novae and soft X-ray transients, we investigate the stability of accretion discs in long-period binary systems. We simulate outbursts due to this thermal-viscous instability for two symbiotic systems, RS~Oph
Externí odkaz:
http://arxiv.org/abs/1804.07916
Context. From stars to active galactic nuclei, many astrophysical systems are surrounded by an equatorial distribution of dusty material that are, in a number of cases, spatially unresolved even with cutting edge facilities. Aims. In this paper, we i
Externí odkaz:
http://arxiv.org/abs/1801.08438
Autor:
Hameury, J. -M., Lasota, J. -P.
Publikováno v:
A&A 602, A102 (2017)
The disc instability model (DIM) has been very successful in explaining the dwarf nova outbursts observed in cataclysmic variables. When, as in intermediate polars (IP), the accreting white dwarf is magnetized, the disc is truncated at the magnetosph
Externí odkaz:
http://arxiv.org/abs/1703.03563
Publikováno v:
A&A 600, A95 (2017)
Context. The disc instability model (DIM) successfully explains why many accreting compact binary systems exhibit outbursts, during which their luminosity increases by orders of magnitude. The DIM correctly predicts which systems should be transient
Externí odkaz:
http://arxiv.org/abs/1701.00472