A dataset provided by the European Space Agency

Name: What causes the dispersion of the O-star X-ray luminosities ?
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 ~ -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 Pollocks 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
Last Update	2025-01-27
Keywords	"log l_x", "parameter space", "magnetic confinement", "rich late type", "bolometric luminosity", "xray properties", "star population", "strongest impact", "magnetic wind confinement", "canonical relation", "natural explanation", "investigations tend"
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 ?', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-loy8ag4