C+ distribution around S 1 in ρ Ophiuchi
نویسندگان
چکیده
منابع مشابه
The Young Stellar Cluster in the Ring Around ρ-Ophiuchi 1. Science Justification
The interaction of newly formed stars with their parent cloud, particularly in the case of massive stars, can have significant consequences for the subsequent development of the cloud. Hot, massive stars will cause cloud disruption through their ionizing flux as well as through the momentum in their stellar winds. Yet, given the right conditions in the cloud, stellar winds may also cause the co...
متن کاملStar Formation in the ρ Ophiuchi Molecular Cloud
A review of star formation in the Rho Ophiuchi molecular complex is presented, with particular emphasis on studies of the main cloud, L1688, since 1991. Recent photometric and parallax measurements of stars in the Upper Scorpius subgroup of the Sco-Cen OB association suggest a distance for the cloud between 120 and 140 parsecs. Star formation is ongoing in the dense cores of L1688 with a median...
متن کاملAccretion in ρ Ophiuchi brown dwarfs : infrared hydrogen line ratios ⋆
Context. Mass accretion rate determinations are fundamental for an understanding of the evolution of pre-main sequence star circumstellar disks. Aims. Magnetospheric accretion models are used to derive values of the mass accretion rates in objects of very different properties, from brown dwarfs to intermediate-mass stars; we test the validity of these models in the brown dwarf regime, where the...
متن کاملCentimeter-wave continuum radiation from the ρ Ophiuchi molecular cloud
The ρ Oph molecular cloud is undergoing intermediate-mass star formation. UV radiation from its hottest young stars heats and dissociates exposed layers, but does not ionize hydrogen. Only faint radiation from the Rayleigh-Jeans tail of ∼ 10–100 K dust is expected at wavelengths longwards of ∼3 mm. Yet Cosmic Background Imager (CBI) observations reveal that the ρ Oph W photo-dissociation region...
متن کاملCentimetre-wave continuum radiation from the ρ Ophiuchi molecular cloud
The ρ Oph molecular cloud is undergoing intermediate-mass star formation. Ultraviolet radiation from its hottest young stars heats and dissociates exposed layers, but does not ionize hydrogen. Only faint radiation from the Rayleigh-Jeans tail of ∼10–100 K dust is expected at wavelengths longwards of ∼3 mm. Yet cosmic background imager (CBI) observations reveal that the ρ Oph W photodissociation...
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ژورنال
عنوان ژورنال: Astronomy & Astrophysics
سال: 2018
ISSN: 0004-6361,1432-0746
DOI: 10.1051/0004-6361/201832953