A dataset provided by the European Space Agency

Name: X-ray Evolution of Classical Novae: Timescales for the SSS Phase
Published: 2008-05-01T00:00:00Z

Proposal ID	040443
Title	X-ray Evolution of Classical Novae: Timescales for the SSS Phase
Download Data Associated to the proposal	https://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0404430201 https://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0404430301 https://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0404430401 https://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0404430501 https://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0404431101 https://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0404431201
DOI	https://doi.org/10.5270/esa-ym27rhe
Principal Investigator, PI	Dr Guy Stringfellow
Abstract	The outbursts of novae are driven by a thermonuclear runaway at the base of anaccreted shell. Soft X-ray emission resulting from high surface temperatures onthe WD after outburst are expected, but seldom observed (SSS phase). Some novaeenter the SSS phase within the first year after outburst, and quickly turn offthereafter (the very fast ONeMg novae). Others (e.g., slow novae) are delayedyears after outburst before entering the SSS stage, which then lasts many years.ROSAT detected only 3 novae in their SSS state; XMM has observed 5, 3 which haveSSS spectrums. Insight into the diversity and evolution of novae can be gainedby determining when (or if) the SSS stage begins, when turnoff occurs, and howthis relates to composition and the mass of the WD.
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 The XMM Cluster Survey: optical analysis methodology and the first data release \|Mehrtens Nicola Romer A. Kathy et al. \| MNRAS \| 423-1024 \| 2012 \| 2012MNRAS.423.1024M \| http://ui.adsabs.harvard.edu/#abs/2012MNRAS.423.1024M General X-ray properties of hot massive stars \|Naze Yael \| BSRSL \| 80-109 \| 2011 \| 2011BSRSL..80..109N \| http://ui.adsabs.harvard.edu/#abs/2011BSRSL..80..109N The XMM Cluster Survey: X-ray analysis methodology \|Lloyd-Davies E. J. Romer A. Kathy et al. \| MNRAS \| 418-14 \| 2011 \| 2011MNRAS.418...14L \| http://ui.adsabs.harvard.edu/#abs/2011MNRAS.418...14L 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 Sunyaev-Zeldovich effect or not? Detecting the main foreground effect of most galaxy clusters \|Xiao Weike Chen Chen et al. \| MNRAS \| 432-41 \| 2013 \| 2013MNRAS.432L..41X \| http://ui.adsabs.harvard.edu/#abs/2013MNRAS.432L..41X The population of X-ray supernova remnants in the Large Magellanic Cloud \|Maggi P. Haberl F. et al. \| A&A \| 585-162 \| 2016 \| 2016A&A...585A.162M \| http://ui.adsabs.harvard.edu/#abs/2016A&A...585A.162M 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 Identification of high-mass X-ray binaries selected from XMM-Newton observations of the LMC* \|van Jaarsveld N. Buckley D. A. H. et al. \| MNRAS \| 475-3253 \| 2018 \| 2018MNRAS.475.3253V \| http://ui.adsabs.harvard.edu/#abs/2018MNRAS.475.3253V Anisotropy of the galaxy cluster X-ray luminosity-temperature relation \|Migkas Konstantinos Reiprich Thomas H. \| A&A \| 611-50 \| 2018 \| 2018A&A...611A..50M \| http://ui.adsabs.harvard.edu/#abs/2018A&A...611A..50M The XMM Cluster Survey: Present status and latest results \|Viana P. T. P. Mehrtens N. et al. \| AN \| 334-462 \| 2013 \| 2013AN....334..462V \| http://ui.adsabs.harvard.edu/#abs/2013AN....334..462V X-Ray Luminosity and Size Relationship of Supernova Remnants in the LMC \|Ou Po-Sheng Chu You-Hua et al. \| ApJ \| 863-137 \| 2018 \| 2018ApJ...863..137O \| http://ui.adsabs.harvard.edu/#abs/2018ApJ...863..137O Testing emergent gravity on galaxy cluster scales \|Tamosiunas Andrius Bacon David et al. \| JCAP \| 5-53 \| 2019 \| 2019JCAP...05..053T \| http://ui.adsabs.harvard.edu/#abs/2019JCAP...05..053T Chandra Follow-up of the SDSS DR8 Redmapper Catalog Using the MATCha Pipeline \|Hollowood Devon L. Jeltema Tesla et al. \| ApJS \| 244-22 \| 2019 \| 2019ApJS..244...22H \| http://ui.adsabs.harvard.edu/#abs/2019ApJS..244...22H Stellar mass as a galaxy cluster mass proxy: application to the Dark Energy Survey redMaPPer clusters \|Palmese A. Annis J. et al. \| MNRAS \| 493-4591 \| 2020 \| 2020MNRAS.493.4591P \| http://ui.adsabs.harvard.edu/#abs/2020MNRAS.493.4591P New optically identified supernova remnants in the Large Magellanic Cloud \|Yew Miranda Filipoviu0107 Miroslav D. et al. \| MNRAS \| 500-2336 \| 2021 \| 2021MNRAS.500.2336Y \| http://ui.adsabs.harvard.edu/#abs/2021MNRAS.500.2336Y 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 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	2006-12-02T20:25:39Z/2007-04-13T18:21:39Z
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	2008-05-01T00:00:00Z
Last Update	2025-01-27
Keywords	"novae enter", "x ray evolution", "sss stage", "accreted shell", "sss phase", "fast onemg novae", "turnoff occurs", "ROSAT", "thermonuclear runaway", ".", "XMM", "soft xray emission", "surface temperatures", " slow novae", "sss spectrums", "classical novae"
Publisher And Registrant	European Space Agency
Credit Guidelines	European Space Agency, Dr Guy Stringfellow, 2008, 'X-ray Evolution of Classical Novae: Timescales for the SSS Phase', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-ym27rhe