Observational signatures of outbursting protostars - I: From hydrodynamic simulations to observations
Abstract Accretion onto protostars may occur in sharp bursts. Accretion bursts during the embedded phase of young protostars are probably most intense, but can only be inferred indirectly through long-wavelength observations. We perform radiative transfer calculations for young stellar objects (YSOs...
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Published in | Monthly notices of the Royal Astronomical Society Vol. 487; no. 4; pp. 5106 - 5117 |
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Main Authors | , , , , , , , |
Format | Journal Article |
Language | English |
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21.08.2019
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Abstract | Abstract
Accretion onto protostars may occur in sharp bursts. Accretion bursts during the embedded phase of young protostars are probably most intense, but can only be inferred indirectly through long-wavelength observations. We perform radiative transfer calculations for young stellar objects (YSOs) formed in hydrodynamic simulations to predict the long wavelength, sub-mm and mm, flux responses to episodic accretion events, taking into account heating from the young protostar and from the interstellar radiation field. We find that the flux increase due to episodic accretion events is more prominent at sub-mm wavelengths than at mm wavelengths; e.g. a factor of ∼570 increase in the luminosity of the young protostar leads to a flux increase of a factor of 47 at 250 $\mu$m but only a factor of 10 at 1.3 mm. Heating from the interstellar radiation field may reduce further the flux increase observed at longer wavelengths. We find that during FU Ori-type outbursts the bolometric temperature and luminosity may incorrectly classify a source as a more evolved YSO due to a larger fraction of the radiation of the object being emitted at shorter wavelengths. |
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AbstractList | Abstract
Accretion onto protostars may occur in sharp bursts. Accretion bursts during the embedded phase of young protostars are probably most intense, but can only be inferred indirectly through long-wavelength observations. We perform radiative transfer calculations for young stellar objects (YSOs) formed in hydrodynamic simulations to predict the long wavelength, sub-mm and mm, flux responses to episodic accretion events, taking into account heating from the young protostar and from the interstellar radiation field. We find that the flux increase due to episodic accretion events is more prominent at sub-mm wavelengths than at mm wavelengths; e.g. a factor of ∼570 increase in the luminosity of the young protostar leads to a flux increase of a factor of 47 at 250 $\mu$m but only a factor of 10 at 1.3 mm. Heating from the interstellar radiation field may reduce further the flux increase observed at longer wavelengths. We find that during FU Ori-type outbursts the bolometric temperature and luminosity may incorrectly classify a source as a more evolved YSO due to a larger fraction of the radiation of the object being emitted at shorter wavelengths. |
Author | Stamatellos, Dimitris Baek, Giseon Herczeg, Gregory MacFarlane, Benjamin Chen, Huei-Ru Vivien Lee, Jeong-Eun Kang, Sung-Ju Johnstone, Doug |
Author_xml | – sequence: 1 givenname: Benjamin surname: MacFarlane fullname: MacFarlane, Benjamin organization: Jeremiah Horrocks Institute for Mathematics, Physics and Astronomy, University of Central Lancashire, Preston PR1 2HE, UK – sequence: 2 givenname: Dimitris orcidid: 0000-0002-4502-8344 surname: Stamatellos fullname: Stamatellos, Dimitris organization: Jeremiah Horrocks Institute for Mathematics, Physics and Astronomy, University of Central Lancashire, Preston PR1 2HE, UK – sequence: 3 givenname: Doug surname: Johnstone fullname: Johnstone, Doug organization: NRC Herzberg Astronomy and Astrophysics, 5071 West Saanich Rd, Victoria V9E 2E7, Canada, Department of Physics and Astronomy, University of Victoria, Victoria V8P 1A1, Canada – sequence: 4 givenname: Gregory surname: Herczeg fullname: Herczeg, Gregory organization: Kavli Institute for Astronomy and Astrophysics, Peking University, Yiheyuan 5, Haidian Qu, 100871 Beijing, China – sequence: 5 givenname: Giseon surname: Baek fullname: Baek, Giseon organization: School of Space Research and Institute of Natural Sciences, Kyung Hee University, 1732 Deogyeong-daero, Giheung-gu, Yongin-si, Gyeonggi-do 446-701, Republic of Korea – sequence: 6 givenname: Huei-Ru Vivien surname: Chen fullname: Chen, Huei-Ru Vivien organization: Department of Physics & Astornomy, National Tsing Hua University, Kuang Fu Road, Hsinchu, 30013 Taiwan – sequence: 7 givenname: Sung-Ju surname: Kang fullname: Kang, Sung-Ju organization: Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Republic of Korea – sequence: 8 givenname: Jeong-Eun surname: Lee fullname: Lee, Jeong-Eun organization: School of Space Research and Institute of Natural Sciences, Kyung Hee University, 1732 Deogyeong-daero, Giheung-gu, Yongin-si, Gyeonggi-do 446-701, Republic of Korea |
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Accretion onto protostars may occur in sharp bursts. Accretion bursts during the embedded phase of young protostars are probably most intense, but can... |
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Title | Observational signatures of outbursting protostars - I: From hydrodynamic simulations to observations |
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