Model of the vibrationally excited HO maser at 658 GHz in circumstellar envelopes around asymptotic giant branch stars
arXiv:1503.07041 · doi:10.1093/mnras/stv485
Abstract
The model is presented of HO maser in the line within the first excited vibrational state of the molecule around oxygen-rich asymptotic giant branch stars. It is suggested that the maser cloud is located in the inner layers of the circumstellar envelope where intense dust formation takes place. The calculations took into account rotational levels belonging to the five lowest vibrational states of the HO molecule. The model predicts the gain values of the 658-GHz maser about cm at H molecule concentrations cm and at high ortho-HO concentrations cm. The gas temperatures K are considered to be a necessary condition for the effective maser operation. Results are presented for other maser transitions of the excited vibrational states of the molecule.
9 pages, 5 figures, accepted for publication in MNRAS. arXiv admin note: text overlap with arXiv:1309.7547
References in corpus (10)
- A close halo of large transparent grains around extreme red giant stars
- Quasi-classical rate coefficient calculations for the rotational (de)excitation of H2O by H2
- 2D Models for Dust-driven AGB Star Winds
- Exploring wind-driving dust species in cool luminous giants I. Basic criteria and dynamical models of M-type AGB stars
- ALMA sub-mm maser and dust distribution of VY Canis Majoris
- Submillimeter vibrationally excited water emission from the peculiar red supergiant VY CMa
- Circumstellar water vapour in M-type AGB stars: Constraints from H2O(1_10 - 1_01) lines obtained with Odin
- Late Stages of Stellar Evolution - Herschel's contributions
- Water vapor emission from IRC+10216 and other carbon-rich stars: model predictions and prospects for multitransition observations
- H_2^{16}O and H_2^{18}O Maser Emission from Gas-Dust Clouds