Short-period X-ray oscillations in super-soft novae and persistent super-soft sources

Journal article
(other)


Publication Details

Author(s): Ness JU, Beardmore AP, Osborne JP, Kuulkers E, Henze M, Piro AL, Drake JJ, Dobrotka A, Schwarz G, Starrfield S, Kretschmar P, Hirsch M, Wilms J
Journal: Astronomy & Astrophysics
Publisher: EDP Sciences
Publication year: 2015
Volume: 578
ISSN: 0004-6361


Abstract

Conclusions. Since fast rotation periods of the white dwarfs as origin of these transient oscillations are speculative, we concentrate on pulsation mechanisms. We present initial considerations predicting the oscillation period to scale linearly with the white dwarf radius (and thus mass), weakly with the pressure at the base, and luminosity. Estimates of the size of the white dwarf could be useful for determining whether these systems are more massive than typical white dwarfs, and thus whether they are growing from accretion over time. Signs of such mass growth may have implications for whether some of these systems are attractive as Type Ia supernova progenitors.


FAU Authors / FAU Editors

Hirsch, Maria
Dr.Karl-Remeis-Sternwarte Bamberg, Astronomisches Institut
Wilms, Jörn Prof. Dr.
Professur für Astronomie und Astrophysik


External institutions with authors

American Astronomical Society
Arizona State University (ASU)
California Institute of Technology (Caltech)
European Space Astronomy Centre (ESAC)
Harvard University
Slovak university of technology in Bratislava
University of Leicester


How to cite

APA:
Ness, J.-U., Beardmore, A.P., Osborne, J.P., Kuulkers, E., Henze, M., Piro, A.L.,... Wilms, J. (2015). Short-period X-ray oscillations in super-soft novae and persistent super-soft sources. Astronomy & Astrophysics, 578. https://dx.doi.org/10.1051/0004-6361/201425178

MLA:
Ness, J-U, et al. "Short-period X-ray oscillations in super-soft novae and persistent super-soft sources." Astronomy & Astrophysics 578 (2015).

BibTeX: 

Last updated on 2019-26-04 at 15:08