Zobrazeno 1 - 10
of 731
pro vyhledávání: '"emission-line [Stars]"'
Autor:
Ilfa A. Gabitova, Anatoly S. Miroshnichenko, Sergey V. Zharikov, Ainash Amantayeva, Serik A. Khokhlov
Publikováno v:
Galaxies, Vol 12, Iss 3, p 23 (2024)
κ Draconis is a binary system with a classical Be star as the primary component. Its emission-line spectrum consists of hydrogen lines, notably the Hα line with peak intensity ratio (V/R) variations phase-locked with the orbital period P = 61.55 da
Externí odkaz:
https://doaj.org/article/21041d2b9f0a45129e3357b01cd8d589
Autor:
A. S. Nodyarov, A. S. Miroshnichenko, S. A. Khokhlov, S. V. Zharikov, A. T. Agishev, I. A. Gabitova, N. L. Vaidman, N. Manset
Publikováno v:
The Astrophysical Journal, Vol 968, Iss 2, p 52 (2024)
HD 327083 is a binary system that consists of two supergiant components and exhibits the B[e] phenomenon. In this paper, we report the determination of a new set of the system’s fundamental parameters using a combination of photometric and spectros
Externí odkaz:
https://doaj.org/article/c141376cb64c43c3b9a440157243043b
Autor:
Serat Saad, Kaitlyn Lane, Marina Kounkel, Keivan G. Stassun, Ricardo López-Valdivia, Jinyoung Serena Kim, Karla Peña Ramírez, Guy S. Stringfellow, Carlos G. Román-Zúñiga, Jesús Hernández, Scott J. Wolk, Lynne A. Hillenbrand
Publikováno v:
The Astronomical Journal, Vol 167, Iss 3, p 125 (2024)
We developed a tool that measures equivalent widths of various lines in low-resolution optical spectra, and it was applied to stellar spectra obtained as part of SDSS-V and LAMOST programs. These lines, such as Li i, which directly indicates stellar
Externí odkaz:
https://doaj.org/article/348265a21411476ea7aa2c5c88e5181e
Akademický článek
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Autor:
Anatoly S. Miroshnichenko, Raghav Chari, Stephen Danford, Peter Prendergast, Alicia N. Aarnio, Ivan L. Andronov, Lidiia L. Chinarova, Aidan Lytle, Ainash Amantayeva, Ilfa A. Gabitova, Nadezhda L. Vaidman, Sayat S. Baktybayev, Serik A. Khokhlov
Publikováno v:
Galaxies, Vol 11, Iss 4, p 83 (2023)
There is growing evidence that many Be stars are parts of binary systems. As the B-type primaries are very fast rotators and their spectral lines may be distorted by the circumstellar material, it is not easy to measure their radial velocity directly
Externí odkaz:
https://doaj.org/article/0939e0c53bc9493280fb00a80a5eb955
Publikováno v:
The Astrophysical Journal Letters, Vol 942, Iss 1, p L6 (2022)
The origin of the bright and hard X-ray emission flux among the γ Cas subgroup of B-emission line (Be) stars may be caused by gas accretion onto an orbiting white dwarf (WD) companion. Such Be+WD binaries are the predicted outcome of a second stage
Externí odkaz:
https://doaj.org/article/e7ddcac8590246d992474eeffe73702e
Autor:
Anatoly S. Miroshnichenko, Sergei V. Zharikov, Nadine Manset, Serik A. Khokhlov, Atilkhan S. Nodyarov, Valentina G. Klochkova, Stephen Danford, Aizhan K. Kuratova, Ronald Mennickent, S. Drew Chojnowski, Ashish Raj, Devendra Bisht
Publikováno v:
Galaxies, Vol 11, Iss 1, p 36 (2023)
This paper describes recent studies of the FS CMa-type objects, a group of stars showing the B[e] phenomenon defined in 2007. The objects exhibit strong emission-line spectra with both permitted and forbidden lines suggesting the presence of a B-type
Externí odkaz:
https://doaj.org/article/62874464d315484297c18fa31aa520ab
Autor:
Nolan Matthews, Jean-Pierre Rivet, David Vernet, Mathilde Hugbart, Guillaume Labeyrie, Robin Kaiser, Julien Chabé, Clément Courde, Olivier Lai, Farrokh Vakili, Olivier Garde, William Guerin
Publikováno v:
The Astronomical Journal, Vol 165, Iss 3, p 117 (2023)
We report on observations of the extended environment of the bright Be star γ -Cas performed using intensity interferometry measurements within its H α emission line. These observations were performed using a modified version of the I2C intensity i
Externí odkaz:
https://doaj.org/article/6efccd6f5ec34090811613aef73498cb
Publikováno v:
The Astronomical Journal, Vol 165, Iss 5, p 203 (2023)
Close binary interactions may play a critical role in the formation of the rapidly rotating Be stars. Mass transfer can result in a mass gainer star spun up by the accretion of mass and angular momentum, while the mass donor is stripped of its envelo
Externí odkaz:
https://doaj.org/article/3acd7db633654a9dba2dd6288bf32488
Akademický článek
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