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K-band High-Resolution Spectroscopy of Embedded Massive Protostars
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K-band High-Resolution Spectroscopy of Embedded Massive Protostars
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Paper
K-band High-Resolution Spectroscopy of Embedded Massive Protostars
2021
Overview
A classical paradox in high-mass star formation is that powerful radiation pressure can halt accretion, preventing further growth of a central star. Disk accretion has been proposed to solve this problem, but the disks and the accretion process in high-mass star formation are poorly understood. We executed high-resolution (\\(R\\)=35,000-70,000) iSHELL spectroscopy in \\(K\\)-band for eleven high-mass protostars. Br-\\(\\) emission was observed toward eight sources, and the line profiles for most of these sources are similar to those of low-mass PMS stars. Using an empirical relationship between the Br-\\(\\) and accretion luminosities, we tentatively estimate disk accretion rates ranging from \\(\\)10\\(^-8\\) and \\(\\)10\\(^-4\\) \\(M_\\) yr\\(^-1\\). These low-mass-accretion rates suggest that high-mass protostars gain more mass via episodic accretion as proposed for low-mass protostars. Given the detection limits, CO overtone emission (\\(v\\)=2-0 and 3-1), likely associated with the inner disk region (\\(r 100\\) au), was found towards two sources. This low-detection rate compared with Br-\\(\\) emission is consistent with previous observations. Ten out of the eleven sources show absorption at the \\(v\\)=0-2 \\( R(7)-R(14)\\) CO R-branch. Most of them are either blueshifted or redshifted, indicating that the absorption is associated with an outflow or an inflow with a velocity of up to \\(50\\) km s\\(^-1\\). Our analysis indicates that the absorption layer is well thermalized (and therefore \\(n_ H_2 10^6\\) cm\\(^-3\\)) at a single temperature of typically 100-200 K, and located within 200-600 au of the star.
Publisher
Cornell University Library, arXiv.org
