A dataset provided by the European Space Agency

Name: What causes the dispersion of the O-star X-ray luminosities questionMark
Published: 2013-01-27T00:00:00Z

Proposal ID	067206
Title	What causes the dispersion of the O-star X-ray luminosities ?
Download Data Associated to the proposal	https://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0672060101
DOI	https://doi.org/10.5270/esa-loy8ag4
Principal Investigator, PI	Dr Hugues Sana
Abstract	O-type X-ray luminosity scales with their bolometric luminosity according tocanonical relation: log L_X/L_bol virgul -7. Yet, significant dispersion is observedaround this relation. Binarity was often considered as a natural explanation tothe observed dispersion but recent investigations tend to disprove thisstatement. We propose to investigate the impact of magnetic wind confinement onthe X-ray properties of O stars, and whether or not it can explain the spreadaround the canonical relation. The nearby young open cluster, IC2944, hosts arich late-type O-star population and is ideally suited for our purpose. It willallow us to investigate with unprecedented details a region of the parameterspace where magnetic confinement is expected to have the strongest impact.
Publications	X-ray properties of the young open clusters HM1 and IC 2944/2948 \|Naze, Y., Rauw, G., et al. \| A&A \| 555-83 \| 2013 \| 2013A&A...555A..83N \| http://ui.adsabs.harvard.edu/#abs/2013A&A...555A..83N Is the Pollock.s paradigm of X-ray emission for O stars correct? \|Ryspaeva, E. B., Kholtygin, A. F., \| AN \| 338-959 \| 2017 \| 2017AN....338..959R \| http://ui.adsabs.harvard.edu/#abs/2017AN....338..959R Analysis of the X-ray emission of OB stars: O stars \|Ryspaeva, Elizaveta, Kholtygin, Alexander, \| RAA \| 18-104 \| 2018 \| 2018RAA....18..104R \| http://ui.adsabs.harvard.edu/#abs/2018RAA....18..104R 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	2012-01-01T09:42:07Z/2012-01-01T21:20:37Z
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	2013-01-27T00:00:00Z
Keywords	"rich late type", "xray properties", "bolometric luminosity", "parameter space", "investigations tend", "magnetic confinement", "strongest impact", "canonical relation", "magnetic wind confinement", "natural explanation", "log l_x", "star population"
Publisher And Registrant	European Space Agency
Credit Guidelines	European Space Agency, Dr Hugues Sana, 2013, 'What causes the dispersion of the O-star X-ray luminosities questionMark', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-loy8ag4