Recent discoveries of supersoft X-ray sources in M 31
| Autor: | Dieter H. Hartmann, Michael Freyberg, Gloria Sala, Holger Stiele, Arne Rau, Margarita Hernanz, Despina Hatzidimitriou, Frank Haberl, Wolfgang Pietsch, Marina Orio, Martin Henze, Jochen Greiner |
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| Jazyk: | angličtina |
| Rok vydání: | 2009 |
| Předmět: |
Physics
High Energy Astrophysical Phenomena (astro-ph.HE) Stars: individual: (M31N 2007-06b M31N 2007-1 1a M31N 2006-04a) individual: (M 31) [Galaxies] X-ray FOS: Physical sciences Astronomy and Astrophysics Astrophysics Orbital period Light curve Monitoring program Galaxy X-rays: binaries Space and Planetary Science Monitoring data Globular cluster Galaxies: individual: (M 31) Novae cataclysmic variables binaries [X-rays] individual: (M31N 2007-06b M31N 2007-1 1a M31N 2006-04a) [Stars] Astrophysics - High Energy Astrophysical Phenomena |
| Zdroj: | Digital.CSIC. Repositorio Institucional del CSIC instname |
| Popis: | Classical novae (CNe) have recently been reported to represent the major class of supersoft X-ray sources (SSSs) in the central area of our neighbouring galaxy M 31. This paper presents a review of results from recent X-ray observations of M 31 with XMM-Newton and Chandra. We carried out a dedicated optical and X-ray monitoring program of CNe and SSSs in the central area of M 31. We discovered the first SSSs in M 31 globular clusters (GCs) and their connection to the very first discovered CN in a M 31 GC. This result may have an impact on the CN rate in GCs. Furthermore, in our optical and X-ray monitoring data we discovered the CN M31N 2007-11a, which shows a very short SSS phase of 29 - 52 days. Short SSS states (durations < 100 days) of CNe indicate massive white dwarfs (WDs) that are candidate progenitors of supernovae type Ia. In the case of M31N 2007-11a, the optical and X-ray light curves suggest a binary containing a WD with M_WD > 1.0 M_sun. Finally, we present the discovery of the SSS counterpart of the CN M31N 2006-04a. The X-ray light curve of M31N 2006-04a shows short-time variability, which might indicate an orbital period of about 2 hours. 4 pages, 1 figure; Proc. of workshop "Supersoft X-ray Sources - New Developments", ESAC, May 2009; accepted for publication in Astronomische Nachrichten |
| Databáze: | OpenAIRE |
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