IRAS observations of the Rho Ophiuchi infrared cluster - Spectral energy distributions and luminosity function

Wilking, B. A.; Lada, Charles J.; Young, E. T.

doi:10.1086/167439

Cited by 328 publications

(322 citation statements)

References 12 publications

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“…In the context of the SIS model, this age suggests that the envelope and the collapsed protostellar core ϩ disk will each contain comparable amounts of material. Alternatively, if we identify 175 AU with the centrifugal balance radius, r c ϭ 0.058a⍀ 0 2 t 3 ϭ 0.030(⍀ 0 /10 Ϫ13 s Ϫ1 ) 2 t 4 3 AU, then the age of the system is less than 1.8 ϫ 10 5 yr, similar to the age estimates for class I sources (Wilking, Lada, & Young 1989). In this picture, the magnetic pseudodisk, if present, would extend to 2300 AU and must have a very low column density in order to be undetectable with lower resolution measurements (e.g., André et al 1993).…”

Section: Discussionmentioning

confidence: 52%

Accretion disks around class 0 protostars: The case of VLA 1623

Wilson¹,

Carlstrom²,

Lay³

et al. 1997

AIP Conference Proceedings

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Continuum emission at 220 and 355 GHz from the prototype class 0 source VLA 1623 has been detected using the James Clerk Maxwell Telescope-Caltech Submillimeter Observatory interferometer. Gaussian fits to the data place an upper limit of 70 AU on the half-width at half-maximum radius of the emission, which implies an upper limit of 1175 AU for the cutoff radius of the circumstellar disk in the system. In the context of existing collapse models, this disk could be magnetically supported on the largest scales and have an age of 16 ϫ 10 4 yr, consistent with previous suggestions that class 0 sources are quite young. The innermost region of the disk within 16 AU is likely to be in centrifugal support, which is likely large enough to provide a drive for the outflow according to current theoretical models. Alternatively, if 175 AU corresponds to the centrifugal radius of the disk, the age of the system is 12 ϫ 10 5 yr, closer to age estimates for class I sources.

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Section: Discussionmentioning

confidence: 52%

Accretion disks around class 0 protostars: The case of VLA 1623

Wilson¹,

Carlstrom²,

Lay³

et al. 1997

AIP Conference Proceedings

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“…This indicates lower levels of accretion from the debris disc than is occurring in earlier stages. Class III lifetimes, as derived from counting statistics, are found to be similar to Class II objects, on the order of 10 6 years (Wilking et al 1989). A Class III object has an IR spectral index α 2: it can be modelled as a reddened blackbody (Wilking et al 1989).…”

Section: Class IImentioning

confidence: 85%

“…The evolutionary state of a protostellar source can be inferred from its spectral index using the system proposed for Class I-III sources by Wilking et al (1989), and extended to Class 0 (André et al 1993;André 1994), and to sources with flat spectral indices, which lie between Class I and Class II (Greene et al 1994). Alternatively, a source can be classified using its bolometric temperature, as calculated for a blackbody distribution with the same mean frequency as the source's spectral energy distribution (Chen et al 1995).…”

Section: Protostarsmentioning

confidence: 99%

“…The system is detectable in infrared emission, but the protostar is deeply embedded and the emission is still dominated by the envelope. A Class I source has a lifetime 5 × 10 5 years, determined from the observed ratio of Class I sources to T Tauri stars (Wilking et al 1989;Dunham et al 2014 and references therein).…”

Section: Class Imentioning

confidence: 99%

“…The star has a bolometric temperature in the range 650 − 2880 K. A Class II object has a broader-than-blackbody energy distribution with flat or decreasing emission long-ward of 2µm (e.g. Wilking et al 1989). …”

Section: Class IImentioning

confidence: 99%

See 2 more Smart Citations

Submillimetre Studies of Prestellar and Starless Cores in the Ophiuchus, Taurus and Cepheus Molecular Clouds

Pattle¹

2017

Springer Theses

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Spectroscopic and photometric behavior of LP Ori

Elmaslı,

Ünal,

Özuyar

2024

Astron Nachr

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We performed spectroscopic and photometric analyses on the early B‐type LP Ori young stellar object located in the Orion Nebula. The high‐resolution spectra of LP Ori was obtained at the Ankara University Kreiken Observatory in 2023, while all spectra recorded over the past 19 years were extracted from the ESO and ESPaDOnS archives. In these spectra of LP Ori, there is typically an emission observed in the core of the Balmer profile. This structure is accompanied by a 14‐year interval inverse P‐Cygni repetition superimposed on the Balmer profile. Additionally, an emission in the 5,875 He I line is visible in the spectra in the year 2023. When this emission is considered together with the inverse P‐Cygni structures, these observations suggest that LP Ori is a Herbig Ae/Be star. The abundance pattern of LP Ori is close to solar with the exception of a slightly rich helium and slightly poor aluminum abundance. Additionally, the spectral energy distribution of LP Ori was constructed to confirm the infrared excess caused by its circumstellar disk. Furthermore, the photometric analysis performed on the TESS observations of LP Ori shows significant photometric variability and the frequency analysis reveals a Cephei star in its forthcoming evolution.

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IRAS observations of the Rho Ophiuchi infrared cluster - Spectral energy distributions and luminosity function

Cited by 328 publications

References 12 publications

Accretion disks around class 0 protostars: The case of VLA 1623

Accretion disks around class 0 protostars: The case of VLA 1623

Submillimetre Studies of Prestellar and Starless Cores in the Ophiuchus, Taurus and Cepheus Molecular Clouds

Spectroscopic and photometric behavior of LP Ori

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