Binary star orbits from speckle interferometry. 5: A combined speckle/spectroscopic study of the O star binary 15 Monocerotis

Gies, Douglas R.; Mason, Brian D.; Hartkopf, William I.; McAlister, Harold A.; Frazin, R. A.; Hahula, M. E.; Penny, Laura R.; Thaller, M.; Fullerton, A. W.; Shara, Michael M.

doi:10.1086/116786

Cited by 46 publications

(41 citation statements)

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“…The long period of this O + O system (about 25 yr, Gies et al 1993) is compatible with the escape of synchrotron radio photons, which agrees with the results of radio observations.…”

Section: Appendix A: the Cataloguesupporting

confidence: 89%

Catalogue of particle-accelerating colliding-wind binaries

Becker

Raucq

2013

A&A

112

138

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Massive systems made of two or more stars are known to be the site for interesting physical processes -including at least in some cases -particle acceleration. Over the past decade, this topic motivated a particular effort to unveil the properties of these systems and characterize the circumstances responsible for the acceleration of particles and the potential role of pre-supernova massive stars in the production of high energy particles in our Galaxy. Although previous studies on this topic were mostly devoted to processes in general, or to a few individual objects in particular, a unified target-oriented census of particle-accelerating colliding-wind binaries (hereafter PACWBs) does not exist yet. This paper aims at making a general and unified census of these systems, emphasizing their main properties. A general discussion includes energetic considerations along with wind properties in relation with non-thermal emission processes that are likely at work in colliding-wind binaries. Finally, some guidelines for future observational and theoretical studies are drawn.

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“…The long period of this O + O system (about 25 yr, Gies et al 1993) is compatible with the escape of synchrotron radio photons, which agrees with the results of radio observations.…”

Section: Appendix A: the Cataloguesupporting

confidence: 89%

Catalogue of particle-accelerating colliding-wind binaries

Becker

Raucq

2013

A&A

112

138

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“…10 is distinguished by the presence of the massive binary S Mon (the primary component is an O7 V star and the secondary component is an O9.5 V star; Gies et al 1993). This is the only O-type star included in the population of the region, while another two dozen B-type stars are distributed within the cluster, and especially across the S Mon and Cone regions (Dahm 2008).…”

Section: Impact Of Environmental Conditions On Disk Evolutionmentioning

confidence: 99%

The Gaia-ESO Survey and CSI 2264: Substructures, disks, and sequential star formation in the young open cluster NGC 2264

Venuti

Prisinzano

Sacco

et al. 2017

A&A

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Context. Reconstructing the structure and history of young clusters is pivotal to understanding the mechanisms and timescales of early stellar evolution and planet formation. Recent studies suggest that star clusters often exhibit a hierarchical structure, possibly resulting from several star formation episodes occurring sequentially rather than a monolithic cloud collapse. Aims. We aim to explore the structure of the open cluster and star-forming region NGC 2264 ("3 Myr), which is one of the youngest, richest and most accessible star clusters in the local spiral arm of our Galaxy; we link the spatial distribution of cluster members to other stellar properties such as age and evolutionary stage to probe the star formation history within the region. Methods. We combined spectroscopic data obtained as part of the Gaia-ESO Survey (GES) with multi-wavelength photometric data from the Coordinated Synoptic Investigation of NGC 2264 (CSI 2264) campaign. We examined a sample of 655 cluster members, with masses between 0.2 and 1.8 M d and including both disk-bearing and disk-free young stars. We used T eff estimates from GES and g, r, i photometry from CSI 2264 to derive individual extinction and stellar parameters. Results. We find a significant age spread of 4-5 Myr among cluster members. Disk-bearing objects are statistically associated with younger isochronal ages than disk-free sources. The cluster has a hierarchical structure, with two main blocks along its latitudinal extension. The northern half develops around the O-type binary star S Mon; the southern half, close to the tip of the Cone Nebula, contains the most embedded regions of NGC 2264, populated mainly by objects with disks and ongoing accretion. The median ages of objects at different locations within the cluster, and the spatial distribution of disked and non-disked sources, suggest that star formation began in the north of the cluster, over 5 Myr ago, and was ignited in its southern region a few Myr later. Star formation is likely still ongoing in the most embedded regions of the cluster, while the outer regions host a widespread population of more evolved objects; these may be the result of an earlier star formation episode followed by outward migration on timescales of a few Myr. We find a detectable lag between the typical age of disk-bearing objects and that of accreting objects in the inner regions of NGC 2264: the first tend to be older than the second, but younger than disk-free sources at similar locations within the cluster. This supports earlier findings that the characteristic timescales of disk accretion are shorter than those of disk dispersal, and smaller than the average age of NGC 2264 (i.e., À3 Myr). At the same time, we note that disks in the north of the cluster tend to be shorter-lived ("2.5 Myr) than elsewhere; this may reflect the impact of massive stars within the region (notably S Mon), that trigger rapid disk dispersal. Conclusions. Our results, consistent with earlier studies on NGC 2264 and other young clusters, suppor...

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“…Markova et al (2004) consider 15 Mon as a Galactic O-type star with a mass of 32 M and T eff = 37 500 K. Speckle measurements of 15 Mon indicated the presence of a companion of spectral type O9.5 V n (e.g. Gies et al 1993). In very high S/N spectra becomes the companion noticeable by very broad underlying components to the strong He i lines.…”

Section: Hd 36879mentioning

confidence: 99%

Exploring the origin of magnetic fields in massive stars

Hubrig

Schöller

Ilyin

et al. 2013

A&A

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Context. Theories on the origin of magnetic fields in massive stars remain poorly developed, because the properties of their magnetic field as function of stellar parameters could not yet be investigated. Additional observations are of utmost importance to constrain the conditions that are conducive to magnetic fields and to determine first trends about their occurrence rate and field strength distribution. Aims. To investigate whether magnetic fields in massive stars are ubiquitous or appear only in stars with a specific spectral classification, certain ages, or in a special environment, we acquired 67 new spectropolarimetric observations for 30 massive stars. Among the observed sample, roughly one third of the stars are probable members of clusters at different ages, whereas the remaining stars are field stars not known to belong to any cluster or association. Methods. Spectropolarimetric observations were obtained during four different nights using the low-resolution spectropolarimetric mode of FOcal Reducer low dispersion Spectrograph (FORS 2) mounted on the 8-m Antu telescope of the VLT. Furthermore, we present a number of follow-up observations carried out with the high-resolution spectropolarimeters SOFIN mounted at the Nordic Optical Telescope (NOT) and HARPS mounted at the ESO 3.6 m between 2008 and 2011. To assess the membership in open clusters and associations, we used astrometric catalogues with the highest quality kinematic and photometric data currently available. Results. The presence of a magnetic field is confirmed in nine stars previously observed with FORS

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Binary star orbits from speckle interferometry. 5: A combined speckle/spectroscopic study of the O star binary 15 Monocerotis

Cited by 46 publications

References 0 publications

Catalogue of particle-accelerating colliding-wind binaries

Catalogue of particle-accelerating colliding-wind binaries

The Gaia-ESO Survey and CSI 2264: Substructures, disks, and sequential star formation in the young open cluster NGC 2264

Exploring the origin of magnetic fields in massive stars

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