<?xml version="1.0" encoding="UTF-8"?><xml><records><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Henze, M.</style></author><author><style face="normal" font="default" size="100%">Pietsch, W.</style></author><author><style face="normal" font="default" size="100%">Haberl, F.</style></author><author><style face="normal" font="default" size="100%">Sala, G.</style></author><author><style face="normal" font="default" size="100%">Hernanz, M.</style></author><author><style face="normal" font="default" size="100%">Hatzidimitriou, D.</style></author><author><style face="normal" font="default" size="100%">Rau, A.</style></author><author><style face="normal" font="default" size="100%">Hartmann, D. H.</style></author><author><style face="normal" font="default" size="100%">Greiner, J.</style></author><author><style face="normal" font="default" size="100%">Orio, M.</style></author><author><style face="normal" font="default" size="100%">Stiele, H.</style></author><author><style face="normal" font="default" size="100%">Freyberg, M. J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Recent discoveries of supersoft X-ray sources in M 31</style></title><short-title><style face="normal" font="default" size="100%">Astronomische Nachrichten</style></short-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Astrophysics - High Energy Astrophysical Phenomena</style></keyword><keyword><style  face="normal" font="default" size="100%">CATACLYSMIC VARIABLES</style></keyword><keyword><style  face="normal" font="default" size="100%">galaxies: individual: (M 31)</style></keyword><keyword><style  face="normal" font="default" size="100%">M31N 2006-04a k)</style></keyword><keyword><style  face="normal" font="default" size="100%">M31N 2007-11a</style></keyword><keyword><style  face="normal" font="default" size="100%">Novae</style></keyword><keyword><style  face="normal" font="default" size="100%">stars: individual: (M31N 2007-06b k</style></keyword><keyword><style  face="normal" font="default" size="100%">X-rays: binaries</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2010</style></year><pub-dates><date><style  face="normal" font="default" size="100%">2010/02/1</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://ui.adsabs.harvard.edu/abs/2010AN....331..193H</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">331</style></volume><pages><style face="normal" font="default" size="100%">193</style></pages><isbn><style face="normal" font="default" size="100%">0004-6337</style></isbn><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">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 &amp;gt; 1.0 M&lt;SUB&gt;\sun&lt;/SUB&gt;. Finally, we present the discovery of the SSS counterpart of the CN M31N 2006-04a k. The X-ray light curve of M31N 2006-04a shows short-time variability, which might indicate an orbital period of about 2 hours. &lt;P /&gt;Partly based on observations with \xmmk, an ESA Science Mission with instruments and contributions directly funded by ESA Member States and NASA.</style></abstract></record></records></xml>