X-ray and optical spectroscopy of the massive young open cluster IC 1805

Rauw, Grégor; Nazé, Yaël

doi:10.1051/0004-6361/201629207

Cited by 16 publications

(6 citation statements)

References 84 publications

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“…Hydrogen recombination lines are observed in emission owing to mass accretion (Muzerolle et al 1998(Muzerolle et al , 2003Fang et al 2013). X-ray is emitted from their hot coronal region (e.g., Flaccomio et al 2003;Caramazza et al 2012;Rauw & Nazé 2016). Based on these properties, the membership of young stars in NGC 2264 has been thoroughly evaluated by a series of multiwavelength studies (Sung et al 1997;Park et al 2000;Sung et al 2004Sung et al , 2008Sung et al , 2009.…”

Section: Selection Of Member Candidatesmentioning

confidence: 99%

A Gaia View on the Star Formation in the Monoceros OB1 and R1 Associations

Lim

Nazé

Yoon

et al. 2022

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Stellar kinematics provides the key to understanding the star formation process. In this respect, we present a kinematic study of the Monoceros OB1 (Mon OB1) and R1 (Mon R1) associations using the recent Gaia data and radial velocities of stars derived from high-resolution spectroscopy and the literature. A total of 728 members are selected using the criteria based on the intrinsic properties of young stars, parallaxes, and proper motions. The spatial distribution and kinematic properties of members show that these associations have distinct substructures. In Mon OB1, we find one northern group and two southern groups. Mon R1 is composed of three small stellar groups that are spatially and kinematically distinct. Some stars are found in a halo around these two associations. We detect patterns of expansion for most stellar groups in the associations. In addition, two stellar groups in Mon OB1 show the signature of rotation, which provides an important constraint on cluster formation. The star formation history of Mon OB1 is slightly revised. Star formation first occurred in the southern region and subsequently in the northern region. Recent star-forming events ignited deeper into the southern region, while some stars are escaping from Mon OB1, forming a halo. Mon R1 might have formed at the same epoch as the formation of the northern group in Mon OB1. Given that star formation is taking place on different scales along a large arc-like structure, Mon OB1 and Mon R1 may be the results of hierarchical star formation.

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Section: Selection Of Member Candidatesmentioning

confidence: 99%

A Gaia View on the Star Formation in the Monoceros OB1 and R1 Associations

Lim

Nazé

Yoon

et al. 2022

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“…One prediction of this scenario is that for the earliest and most luminous O-type stars, featuring dense winds, the L x /L bol relation should saturate and decline with increasing Ṁ (hence with increasing L bol ) because the optical depth of the winds to X-rays becomes significant. Evidence of such an effect has been reported for the O2 If star HD93129A [17] and for the O4 If + star HD15570 [132].…”

Section: Ob Starsmentioning

confidence: 83%

X-ray emission of massive stars and their winds

Rauw¹

2022

Preprint

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Most types of massive stars display X-ray emission that is strongly affected by the properties of their stellar winds. Single non-magnetic OB stars have an X-ray luminosity that scales with their bolometric luminosity and their emission is thought to arise from a distribution of wind-embedded shocks. The lack of significant short-term stochastic variability indicates that the winds consist of a large number of independent fragments. Detailed investigations of temporal variability unveiled a connection between the photosphere and the wind: well-studied O-type stars exhibit a ∼ 10% modulation of their emission on timescales consistent with their rotation period, and a few early B-type pulsators display ∼ 10% modulations of their X-ray flux with the same period as their photospheric pulsations. Unlike OB stars, their evolved descendants (Wolf-Rayet stars and Luminous Blue Variables) lack a well-defined relation between their X-ray and bolometric luminosities, and several subcategories of objects remain undetected. These properties most likely stem from the combined effects of wind optical depth and wind velocity. Magnetic OB stars display an enhanced X-ray emission which is frequently modulated by the rotation of the star. These properties are well explained by the magnetically confined wind shock model and an oblique magnetic rotator configuration. Some massive binaries display phase-dependent excess emission arising from the collision between the winds of the binary components. Yet, the majority of the massive binaries do not show evidence for such an emission, probably as a consequence of radiative cooling of the shock-heated plasma. Finally, a growing subset of the Be stars, the so-called γ Cas stars, feature an unusually hard and strong thermal X-ray emission that varies in a complicated manner over a wide range of timescales. Several scenarios have been proposed to explain these properties, but the origin of the γ Cas phenomenon remains currently one of the major unsolved puzzles in stellar X-ray astrophysics.

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“…Supersonic winds from two stars in relative proximity are expected to interact with each other leading to high Mach number shocks, giving rise to a variety of observational signatures from radio to γ rays. X-rays from "colliding wind binaries" were in fact predicted by Prilutskii & Usov (1976) and Cherepashchuk (1976) two years before the detection of X-rays from massive stars (see, e.g., the review by Rauw & Nazé, 2016).…”

Section: Colliding Windsmentioning

confidence: 95%

X-rays from Stars and Planetary Systems

Drake

2019

Preprint

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reground) spectra of RS Oph obtained on day 13.9 of the 2006 outburst with pro EG) intervals. X-rays from Stars and Planetary SystemsT he Chandra X-ray Observatory has completed a remarkable twenty years in orbit. A large part of the science program of Chandra during this time has involved the study of stars and their planetary systems. This primer aims to give the reader a taste of the enormous range of stellar and planetary astrophysics that Chandra has enabled. Beginning with a tour of the X-ray solar system zoo, including the stunning pulsating X-ray aurorae of Jupiter, we then move on to the hot million degree outer atmospheres of stars like our own Sun, whose X-ray emission is driven by an internal magnetic dynamo. The same emission processes are also vigorously present in the youngest stars, and we highlight some Chandra observations and results on nascent stellar and planetary systems. Chandra surveys and high resolution spectroscopy of massive stars have provided a new window on the means by which they scavenge X-ray emission from their radiatively-driven winds, sometimes modulating this output by strong underlying stellar magnetic fields. We touch upon the evanescent X-radiation from intermediate mass stars before arriving at the inevitable evolutionary end points of all but massive stars, first in energized X-ray emitting planetary nebulae, then in the slowly cooling, soft-X-ray emitting photospheres of white dwarfs. We conclude with white dwarfs in close binary systems, rejuvenated by interaction with a companion and where accretion gives play to a new range of energetic behavior even more spectacular and cataclysmic than the coruscant astrophysical road down which they have travelled.A Primer on Chandra Stellar and Planetary Science HETGS OBSERVATION OF PZ TEL 933 No. 2, 2004 ) and density (n e ) plasma diagnostics for the He-like O VII ion. Left panel: n e = 10 10 cm −3 . Right panel: R ≡ z/(x + y) versus n e for T e = 10 6 K. et et al. (2001a) He-like Ions as Practical Astrophysical Plasma Diagnostics 117

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X-ray and optical spectroscopy of the massive young open cluster IC 1805

Cited by 16 publications

References 84 publications

A Gaia View on the Star Formation in the Monoceros OB1 and R1 Associations

A Gaia View on the Star Formation in the Monoceros OB1 and R1 Associations

X-ray emission of massive stars and their winds

X-rays from Stars and Planetary Systems

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