A dataset provided by the European Space Agency

Name: X-ray Observations of Quiescent Recurrent Novae in CVs
Published: 2011-10-29T00:00:00Z

Proposal ID	065276
Title	X-ray Observations of Quiescent Recurrent Novae in CVs
Download Data Associated to the proposal	https://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0652760101 https://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0652760201
DOI	https://doi.org/10.5270/esa-0j1nhua
Principal Investigator, PI	Dr Koji Mukai
Abstract	For a binary to be a recurrent nova (RN), it must contain a massive white dwarf(WD) near the Chandrasekhar limit, making it a candidate progenitor of type Iasupernova. Although the WD masses and the accretion rates in RNe must all besimilarly high, the X-ray properties of RNe with red-giant donar stars can bewildly different, ranging from hard and luminous (virgul1e34 ergs/s) to softer andsignificantly fainter (below 1e32 ergs/s). Such drastic differences may indicatethat a third parameter, such as the spin period or the core temperature of theWD, may play an important role. Here we propose quiescent X-ray observations of4 RNe in cataclysmicvariable (CV) systems to test if a third parameter indeedexists.
Publications	Swift X-Ray Observations of Classical Novae. II. The Super Soft Source Sample \|Schwarz, Greg J., Ness, Jan-Uwe, et al. \| ApJS \| 197-31 \| 2011 \| 2011ApJS..197...31S \| http://ui.adsabs.harvard.edu/#abs/2011ApJS..197...31S Serendipitous UV source catalogues for 10 years of XMM and 5 years of Swift \|Yershov, V. N., \| Ap&SS \| 354-97 \| 2014 \| 2014Ap&SS.354...97Y \| http://ui.adsabs.harvard.edu/#abs/2014Ap&SS.354...97Y The Million Optical - Radio/X-ray Associations (MORX) Catalogue \|Flesch, Eric W., \| PASA \| 33-52 \| 2016 \| 2016PASA...33...52F \| http://ui.adsabs.harvard.edu/#abs/2016PASA...33...52F Exploring the end states of massive stars using the X-ray emission of neutron stars and supernova remnants \|Prinz, Tobias, \| PhDT \| 0-305 \| 2013 \| 2013PhDT.......305P \| http://ui.adsabs.harvard.edu/#abs/2013PhDT.......305P Classification of 4XMM-DR9 sources by machine learning \|Zhang, Yanxia, Zhao, Yongheng, \| MNRAS \| 503-5263 \| 2021 \| 2021MNRAS.503.5263Z \| http://ui.adsabs.harvard.edu/#abs/2021MNRAS.503.5263Z The XMM-Newton Line Emission Analysis Program (X-LEAP). I. Emission-line Survey of O VII, O VIII, and Fe L-shell Transitions \|Pan, Zeyang, Qu, Zhijie, et al. \| ApJS \| 271-62 \| 2024 \| 2024ApJS..271...62P \| http://ui.adsabs.harvard.edu/#abs/2024ApJS..271...62P From Active Stars to Black Holes: A Discovery Tool for Galactic X-Ray Sources \|Rodriguez, Antonio C., \| PASP \| 136-054201 \| 2024 \| 2024PASP..136e4201R \| http://ui.adsabs.harvard.edu/#abs/2024PASP..136e4201R Robust constraints on feebly interacting particles using XMM-Newton \|Luque, Pedro De la Torre, Balaji, Shyam, \| PhRvD \| 109-L101305 \| 2024 \| 2024PhRvD.109j1305L \| http://ui.adsabs.harvard.edu/#abs/2024PhRvD.109j1305L Multimessenger search for electrophilic feebly interacting particles from supernovae \|Luque, Pedro De la Torre, Balaji, Shyam, \| PhRvD \| 109-103028 \| 2024 \| 2024PhRvD.109j3028L \| http://ui.adsabs.harvard.edu/#abs/2024PhRvD.109j3028L Importance of Cosmic-Ray Propagation on Sub-GeV Dark Matter Constraints \|De la Torre Luque, Pedro, Balaji, Shyam, \| ApJ \| 968-46 \| 2024 \| 2024ApJ...968...46D \| http://ui.adsabs.harvard.edu/#abs/2024ApJ...968...46D
Instrument	EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage	2010-09-20T23:04:57Z/2010-10-06T02:20:41Z
Version	17.56_20190403_1200
Mission Description	The European Space Agencys (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESAs second cornerstone of the Horizon 2000 Science Programme. It carries 3 high throughput X-ray telescopes with an unprecedented effective area, and an optical monitor, the first flown on a X-ray observatory. The large collecting area and ability to make long uninterrupted exposures provide highly sensitive observations. Since Earths atmosphere blocks out all X-rays, only a telescope in space can detect and study celestial X-ray sources. The XMM-Newton mission is helping scientists to solve a number of cosmic mysteries, ranging from the enigmatic black holes to the origins of the Universe itself. Observing time on XMM-Newton is being made available to the scientific community, applying for observational periods on a competitive basis.
Creator Contact	https://www.cosmos.esa.int/web/xmm-newton/xmm-newton-helpdesk
Date Published	2011-10-29T00:00:00Z
Keywords	"1e32 ergs", "accretion rates", "xray properties", "chandrasekhar limit", "core temperature", "wd masses", "quiescent recurrent novae", "cataclysmicvariable cv systems", "candidate progenitor", "spin period", "x ray", "parameter indeed exists", "1e34 ergs", "recurrent nova rn", "type ia supernova", "quiescent xray"
Publisher And Registrant	European Space Agency
Credit Guidelines	European Space Agency, Dr Koji Mukai, 2011, 'X-ray Observations of Quiescent Recurrent Novae in CVs', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-0j1nhua