New insights on the accretion properties of Class 0 protostars from 2 micron spectroscopy
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| Format: | Preprint |
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2024
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| _version_ | 1866916110100594688 |
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| author | Gouellec, Valentin J. M. Le Greene, Thomas P. Hillenbrand, Lynne A. Yates, Zoe |
| author_facet | Gouellec, Valentin J. M. Le Greene, Thomas P. Hillenbrand, Lynne A. Yates, Zoe |
| contents | Sun-like stars are thought to accrete most of their final mass during the protostellar phase, during which the stellar embryo is surrounded by an infalling dense envelope. We present an analysis of 26 $K$-band spectra of Class 0 protostars, which are the youngest protostars. 18 of these are new observations made with the Keck MOSFIRE instrument. HI Br$γ$ , several H$_2$, and CO $Δ\,v\;=\;2$ features are detected and analyzed. We detect Br$γ$ emission in 62%, CO overtone emission in 50%, and H$_2$ emission in 90% of sources. The HI and CO emission is associated with accretion while the H$_2$ lines are consistent with shock excitation indicating jets/outflows. Six objects exhibit photospheric absorption features, with almost no outflow activity, and no detection of the accretion-related Br$γ$ emission line. Comparing these results with archival sample of Class I $K$-band spectra, we find that the CO and Br$γ$ emission lines are systematically more luminous in Class 0s, suggesting the accretion is on average more vigorous in the Class 0 phase. Typically associated with the heated inner accretion disk, the much higher detection rate of CO overtone emission in Class 0s indicate also that episodes of high accretion activity are more frequent in Class 0 systems. The kinematics of the Class 0 CO overtone emission suggest either an accretion-heated inner disk, or material directly infalling onto the central region. This could point toward an accretion mechanism of different nature in Class 0 systems than the typical picture of magnetospheric accretion. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2401_16532 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | New insights on the accretion properties of Class 0 protostars from 2 micron spectroscopy Gouellec, Valentin J. M. Le Greene, Thomas P. Hillenbrand, Lynne A. Yates, Zoe Solar and Stellar Astrophysics Earth and Planetary Astrophysics Astrophysics of Galaxies Sun-like stars are thought to accrete most of their final mass during the protostellar phase, during which the stellar embryo is surrounded by an infalling dense envelope. We present an analysis of 26 $K$-band spectra of Class 0 protostars, which are the youngest protostars. 18 of these are new observations made with the Keck MOSFIRE instrument. HI Br$γ$ , several H$_2$, and CO $Δ\,v\;=\;2$ features are detected and analyzed. We detect Br$γ$ emission in 62%, CO overtone emission in 50%, and H$_2$ emission in 90% of sources. The HI and CO emission is associated with accretion while the H$_2$ lines are consistent with shock excitation indicating jets/outflows. Six objects exhibit photospheric absorption features, with almost no outflow activity, and no detection of the accretion-related Br$γ$ emission line. Comparing these results with archival sample of Class I $K$-band spectra, we find that the CO and Br$γ$ emission lines are systematically more luminous in Class 0s, suggesting the accretion is on average more vigorous in the Class 0 phase. Typically associated with the heated inner accretion disk, the much higher detection rate of CO overtone emission in Class 0s indicate also that episodes of high accretion activity are more frequent in Class 0 systems. The kinematics of the Class 0 CO overtone emission suggest either an accretion-heated inner disk, or material directly infalling onto the central region. This could point toward an accretion mechanism of different nature in Class 0 systems than the typical picture of magnetospheric accretion. |
| title | New insights on the accretion properties of Class 0 protostars from 2 micron spectroscopy |
| topic | Solar and Stellar Astrophysics Earth and Planetary Astrophysics Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2401.16532 |