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26 April 2024 |
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Inner warm disk of ESO H$alpha$ 279A revealed by NA I and CO overtone emission lines | | A-Ran Lyo
; Jongsoo Kim
; Jae-Joon Lee
; Kyoung-Hee Kim
; Jihyun Kang
; Do-Young Byun
; Gregory Mace
; Kimberly R. Sokal
; Chan Park
; Moo-Young
; Heeyoung Oh
; Young Sam Yu
; Jae Sok Oh
; Ueejeong Jeong
; Hwihyun Kim
; Soojong Pak
; Narae Hwang
; Byeong-Gon Park
; Sungho Lee
; Kyle Kaplan
; Hye-In Lee
; Huynh Anh Nguyen Le
; Daniel Jaffe
; | | Date: |
18 Jul 2017 | | Abstract: | We present analysis of near-infrared, high-resolution spectroscopy towards
the Flat-spectrum YSO (Young Stellar Object) ESO H$alpha$ 279a (1.5 solar
mass) in the Serpens star forming region, at the distance of 429 pc. Using the
Immersion GRating INfrared Spectrometer (IGRINS, R=45,000), we detect emission
lines originating from the accretion channel flow, jet, and inner disk.
Specifically, we identify hydrogen Brackett series recombination, [Fe II], [Fe
III], [Fe IV], Ca I, Na I, H2, H2O and CO overtone emission lines. By modeling
five bands of CO overtone emission lines, and the symmetric double-peaked line
profile for Na I emission lines, we find that ESO H$alpha$ 279a has an
actively accreting Keplerian disk. From our Keplerian disk model, we find that
Na I emission lines originate between 0.04 AU and 1.00 AU, while CO overtone
emission lines are from the outer part of disk, in the range between 0.22 AU
and 3.00 AU. It reveals that the neutral atomic Na gas is a good tracer of the
innermost region of the actively accreting disk. We derive a mass accretion
rate of 2-10x10^{-7} M_solar/yr from the measured Br_gamma emission luminosity
of 1.78(+-0.31)x10^{31} erg/s. | | Source: | arXiv, 1707.5488 | | Services: | Forum | Review | PDF | Favorites | |
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