scholarly journals X‐Ray–emitting Young Stars in the Orion Nebula

2002 ◽  
Vol 574 (1) ◽  
pp. 258-292 ◽  
Author(s):  
Eric D. Feigelson ◽  
Patrick Broos ◽  
James A. Gaffney III ◽  
Gordon Garmire ◽  
Lynne A. Hillenbrand ◽  
...  
Keyword(s):  
Young Stars ◽  
Orion Nebula ◽  
X Ray

scholarly journals Rotational Modulation of X‐Ray Emission in Orion Nebula Young Stars

2005 ◽  
Vol 160 (2) ◽  
pp. 450-468 ◽  
Author(s):  
E. Flaccomio ◽  
G. Micela ◽  
S. Sciortino ◽  
E. D. Feigelson ◽  
W. Herbst ◽  
...  
Keyword(s):  
Young Stars ◽  
Orion Nebula ◽  
X Ray ◽  
Rotational Modulation

scholarly journals The EINSTEIN survey of the young stars in the Orion nebula

1987 ◽  
Vol 122 ◽  
pp. 119-120
Author(s):  
Jean-Pierre Caillault ◽  
Saied Zoonematkermani
Keyword(s):  
Young Stars ◽  
Orion Nebula ◽  
Early Type ◽  
X Ray ◽  
Solar Type ◽  
Early Type Stars ◽  
M Stars

We report here on the complete EINSTEIN survey of Orion within the central 2° x 2° region centered on the Trapezium. We present an X-ray mosaic of the Nebula and a complete X-ray catalog (200 sources) for this very young cluster. In addition, we discuss in detail variability, early-type stars, solar-type stars, and K-M stars.

scholarly journals Double trouble: Gaia reveals (proto)planetary systems that may experience more than one dense star-forming environment

2020 ◽  
Vol 501 (1) ◽  
pp. L12-L17
Author(s):  
Christina Schoettler ◽  
Richard J Parker
Keyword(s):  
Planetary Systems ◽  
Young Star ◽  
Young Stars ◽  
Orion Nebula ◽  
External Effects ◽  
Star Forming ◽  
Star Forming Regions ◽  
Ejection Process ◽  
Runaway Stars

ABSTRACT Planetary systems appear to form contemporaneously around young stars within young star-forming regions. Within these environments, the chances of survival, as well as the long-term evolution of these systems, are influenced by factors such as dynamical interactions with other stars and photoevaporation from massive stars. These interactions can also cause young stars to be ejected from their birth regions and become runaways. We present examples of such runaway stars in the vicinity of the Orion Nebula Cluster (ONC) found in Gaia DR2 data that have retained their discs during the ejection process. Once set on their path, these runaways usually do not encounter any other dense regions that could endanger the survival of their discs or young planetary systems. However, we show that it is possible for star–disc systems, presumably ejected from one dense star-forming region, to encounter a second dense region, in our case the ONC. While the interactions of the ejected star–disc systems in the second region are unlikely to be the same as in their birth region, a second encounter will increase the risk to the disc or planetary system from malign external effects.

X‐Ray Emission from Early‐Type Stars in the Orion Nebula Cluster

2005 ◽  
Vol 160 (2) ◽  
pp. 557-581 ◽  
Author(s):  
B. Stelzer ◽  
E. Flaccomio ◽  
T. Montmerle ◽  
G. Micela ◽  
S. Sciortino ◽  
...  
Keyword(s):  
Orion Nebula ◽  
Early Type ◽  
X Ray ◽  
Early Type Stars

scholarly journals X‐Ray and Infrared Observations of Embedded Young Stars in NGC 2264

2005 ◽  
Vol 618 (2) ◽  
pp. 795-809 ◽  
Author(s):  
Theodore Simon ◽  
S. E. Dahm
Keyword(s):  
Young Stars ◽  
Infrared Observations ◽  
X Ray

scholarly journals Magnetic fields, winds and X-rays of massive stars in the Orion nebula cluster

2010 ◽  
Vol 6 (S272) ◽  
pp. 208-209 ◽  
Author(s):  
Véronique Petit ◽  
Gregg A. Wade ◽  
Evelyne Alecian ◽  
Laurent Drissen ◽  
Thierry Montmerle ◽  
...  
Keyword(s):  
Magnetic Fields ◽  
Massive Stars ◽  
Theoretical Models ◽  
Magnetic Star ◽  
X Rays ◽  
Orion Nebula ◽  
X Ray ◽  
Ob Stars ◽  
The Impact ◽  
The Relationship

AbstractIn some massive stars, magnetic fields are thought to confine the outflowing radiatively-driven wind. Although theoretical models and MHD simulations are able to illustrate the dynamics of such a magnetized wind, the impact of this wind-field interaction on the observable properties of a magnetic star - X-ray emission, photometric and spectral variability - is still unclear. The aim of this study is to examine the relationship between magnetism, stellar winds and X-ray emission of OB stars, by providing empirical observations and confronting theory. In conjunction with the COUP survey of the Orion Nebula Cluster, we carried out spectropolarimatric ESPaDOnS observations to determine the magnetic properties of massive OB stars of this cluster.

scholarly journals Do star clusters form in a completely mass-segregated way?

2019 ◽  
Vol 626 ◽  
pp. A79 ◽  
Author(s):  
Václav Pavlík ◽  
Pavel Kroupa ◽  
Ladislav Šubr
Keyword(s):  
Star Clusters ◽  
Point Of View ◽  
High Mass ◽  
Orion Nebula ◽  
Energy Redistribution ◽  
X Ray ◽  
Star Forming ◽  
Independent Observations ◽  
Mass Segregation ◽  
Rule Out

Context. ALMA observations of the Serpens South star-forming region suggest that stellar protoclusters may be completely mass segregated at birth. Independent observations also suggest that embedded clusters form segregated by mass. Aims. As the primordial mass segregation seems to be lost over time, we aim to study on which timescale an initially perfectly mass-segregated star cluster becomes indistinguishable from an initially not mass-segregated cluster. As an example, the Orion Nebula Cluster (ONC) is also discussed. Methods. We used N-body simulations of star clusters with various masses and two different degrees of primordial mass segregation. We analysed their energy redistribution through two-body relaxation to quantify the time when the models agree in terms of mass segregation, which sets in only dynamically in the models that are primordially not mass segregated. A comprehensive cross-matched catalogue combining optical, infrared, and X-ray surveys of ONC members was also compiled and made available. Results. The models evolve to a similar radial distribution of high-mass stars after the core collapse (about half a median two-body relaxation time, trh) and become observationally indistinguishable from the point of view of mass segregation at time τv ≈ 3.3 trh. In the case of the ONC, using the distribution of high-mass stars, we may not rule out either evolutionary scenario (regardless of whether they are initially mass segregated). When we account for extinction and elongation of the ONC, as reported elsewhere, an initially perfectly mass-segregated state seems to be more consistent with the observed cluster.

OPTICAL SPECTROSCOPY OF X-RAY-SELECTED YOUNG STARS IN THE CARINA NEBULA

2015 ◽  
Vol 150 (6) ◽  
pp. 195 ◽  
Author(s):  
Kaushar Vaidya ◽  
Wen-Ping Chen ◽  
Hsu-Tai Lee
Keyword(s):  
Optical Spectroscopy ◽  
Young Stars ◽  
X Ray ◽  
Carina Nebula

scholarly journals X-ray Emission from Massive Stars at the Core of Very Young Clusters

2016 ◽  
Vol 12 (S329) ◽  
pp. 362-365
Author(s):  
Norbert S. Schulz
Keyword(s):  
Massive Stars ◽  
Stellar Winds ◽  
X Rays ◽  
Stellar Clusters ◽  
Orion Nebula ◽  
X Ray ◽  
The Core ◽  
Hot Plasma ◽  
Young Clusters ◽  
Massive Cluster

AbstractMost cores of very young stellar clusters contain one or more massive stars at various evolutionary stages. Observations of the Orion Nebula Cluster, Trumpler 37, NGC 2362, RCW38, NGC 3603 and many others provide the most comprehensive database to study stellar wind properties of these massive cluster stars in X-rays. In this presentation we review some of these observations and results and discuss them in the context of stellar winds and possible evolutionary implications. We argue that in very young clusters such as RCW38 and M17, shock heated remnants of a natal shell could serve as an alternate explanation to the colliding wind paradigm for the hot plasma components in the X-ray spectra.

scholarly journals Bright X‐Ray Flares in Orion Young Stars from COUP: Evidence for Star‐Disk Magnetic Fields?

2005 ◽  
Vol 160 (2) ◽  
pp. 469-502 ◽  
Author(s):  
F. Favata ◽  
E. Flaccomio ◽  
F. Reale ◽  
G. Micela ◽  
S. Sciortino ◽  
...  
Keyword(s):  
Magnetic Fields ◽  
Young Stars ◽  
X Ray
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