Radiative Transfer modeling of EC 53: An Episodically Accreting Class I Young Stellar Object
| Autor: | Gregory J. Herczeg, Dimitris Stamatellos, Carlos Contreras Peña, Giseon Baek, Jeong-Eun Lee, B. A. Macfarlane, Huei-Ru Vivien Chen, Watson P. Varricatt, Doug Johnstone, Klaus W. Hodapp, Sung-ju Kang |
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| Jazyk: | angličtina |
| Rok vydání: | 2020 |
| Předmět: |
010504 meteorology & atmospheric sciences
Serpens Young stellar object Astrophysics::High Energy Astrophysical Phenomena FOS: Physical sciences Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics 01 natural sciences Luminosity 0103 physical sciences Radiative transfer Protostar Astrophysics::Solar and Stellar Astrophysics 010303 astronomy & astrophysics Solar and Stellar Astrophysics (astro-ph.SR) Astrophysics::Galaxy Astrophysics 0105 earth and related environmental sciences Earth and Planetary Astrophysics (astro-ph.EP) Physics Star formation Astronomy and Astrophysics Astrophysics - Astrophysics of Galaxies Accretion (astrophysics) Astrophysics - Solar and Stellar Astrophysics 13. Climate action Space and Planetary Science Astrophysics of Galaxies (astro-ph.GA) Spectral energy distribution Astrophysics::Earth and Planetary Astrophysics Astrophysics - Earth and Planetary Astrophysics |
| Popis: | In the episodic accretion scenario, a large fraction of the protostellar mass accretes during repeated and large bursts of accretion. Since outbursts on protostars are typically identified at specific wavelengths, interpreting these outbursts requires converting this change in flux to a change in total luminosity. The Class I young stellar object EC 53 in the Serpens Main cloud has undergone repeated increases in brightness at 850 $\mu$m that are likely caused by bursts of accretion. In this study, we perform two- and three-dimensional continuum radiative transfer modeling to quantify the internal luminosity rise in EC 53 that corresponds to the factor of $\sim$1.5 enhancement in flux at 850 $\mu$m. We model the spectral energy distribution and radial intensity profile in both the quiescent and outburst phases. The internal luminosity in the outburst phase is $\sim 3.3$ times brighter than the luminosity in the quiescent phase. The radial intensity profile analysis demonstrates that the detected sub-mm flux variation of EC 53 comes from the heated envelope by the accretion burst. We also find that the role of external heating of the EC 53 envelope by the interstellar radiation field is insignificant. Comment: 16 pages, 14 figures, Accepted for publication in ApJ |
| Databáze: | OpenAIRE |
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