The 2014–2017 outburst of the young star ASASSN-13db: A time-resolved picture of a very-low-mass star between EXors and FUors*
Abstract
Context. Accretion outbursts are key elements in star formation. ASASSN-13db is a M5-type star with a protoplanetary disk, the lowest-mass star known to experience accretion outbursts. Since its discovery in 2013, it has experienced two outbursts, the second of which started in November 2014 and lasted until February 2017. Aims. We observe the photometric and spectroscopic behavior of ASASSN-13db during the 2014–2017 outburst. Methods. We use high- and low-resolution spectroscopy and time-resolved photometry from the ASAS-SN survey, the LCOGT and the Beacon Observatory to study the light curve of ASASSN-13db and the dynamical and physical properties of the accretion flow. Results. The 2014–2017 outburst lasted for nearly 800 days. A 4.15 d period in the light curve likely corresponds to rotational modulation of a star with hot spot(s). The spectra demonstrate multiple emission lines with variable inverse P-Cygni profiles and a highly variable blue-shifted absorption below the continuum. Line ratios from metallic emission lines (Fe I/Fe II, Ti I/Ti II) suggest temperatures of ~5800–6000 K in the accretion flow. Conclusions. Photometrically and spectroscopically, the 2014–2017 event displays an intermediate behavior between EXors and FUors. The accretion rate ([$$\dot{M}$$]= 1–3 × 10-7 M⊙/yr), about two orders of magnitude higher than the accretion rate in quiescence, is not vastly different from the accretion rate observed in 2013. The absorption features in the spectra suggest that the system is viewed at a high angle and drives a powerful, non-axisymmetric wind, maybe related to magnetic reconnection. The properties of ASASSN-13db suggest that temperatures lower than those for solar-type stars are needed for modeling accretion in very-low-mass systems. Finally, the rotational modulation during the outburst reveals that accretion-related structures settle after the beginning of the outburst and can be relatively stable and long-lived. Our work also demonstrates the power of time-resolved photometry and spectroscopy to explore the properties of variable and outbursting stars.
- Authors:
-
- Univ. of Dundee (United Kingdom); Univ. of St Andrews (United Kingdom)
- Univ. of Edinburgh, Scotland (United Kingdom); Univ. of Kent, Canterbury (United Kingdom)
- Univ. of Kent, Canterbury (United Kingdom)
- Univ. of Arizona, Tucson, AZ (United States)
- Diego Portales Univ., Santiago (Chile); Millennium Inst. of Astrophysics, Santiago (Chile)
- The Ohio State Univ., Columbus, OH (United States)
- Univ. of St Andrews (United Kingdom)
- Max-Planck-Institut für Astronomie, Heidelberg (Germany)
- Millennium Inst. of Astrophysics, Santiago (Chile) ; The Ohio State Univ., Columbus, OH (United States)
- Pontifical Catholic Univ. of Chile, Santiago (Chile); Max-Planck-Institut für Astronomie, Heidelberg (Germany)
- Carnegie Observatories, Pasadena, CA (United States)
- Publication Date:
- Research Org.:
- Krell Institute, Ames, IA (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC), Advanced Scientific Computing Research (ASCR)
- OSTI Identifier:
- 1547046
- Grant/Contract Number:
- FG02-97ER25308
- Resource Type:
- Accepted Manuscript
- Journal Name:
- Astronomy and Astrophysics
- Additional Journal Information:
- Journal Volume: 607; Journal ID: ISSN 0004-6361
- Publisher:
- EDP Sciences
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; stars: pre-main sequence; stars: variables: T Tauri, Herbig Ae/Be; stars: individual: ASASSN-13db; stars: low-mass; protoplanetary disks; techniques: spectroscopic
Citation Formats
Sicilia-Aguilar, A., Oprandi, A., Froebrich, D., Fang, M., Prieto, J. L., Stanek, K., Scholz, A., Kochanek, C. S., Henning, Th., Gredel, R., Holoien, T. W. -. S., Rabus, M., Shappee, B. J., Billington, S. J., Campbell-White, J., and Zegmott, T. J. The 2014–2017 outburst of the young star ASASSN-13db: A time-resolved picture of a very-low-mass star between EXors and FUors*. United States: N. p., 2017.
Web. doi:10.1051/0004-6361/201731263.
Sicilia-Aguilar, A., Oprandi, A., Froebrich, D., Fang, M., Prieto, J. L., Stanek, K., Scholz, A., Kochanek, C. S., Henning, Th., Gredel, R., Holoien, T. W. -. S., Rabus, M., Shappee, B. J., Billington, S. J., Campbell-White, J., & Zegmott, T. J. The 2014–2017 outburst of the young star ASASSN-13db: A time-resolved picture of a very-low-mass star between EXors and FUors*. United States. https://doi.org/10.1051/0004-6361/201731263
Sicilia-Aguilar, A., Oprandi, A., Froebrich, D., Fang, M., Prieto, J. L., Stanek, K., Scholz, A., Kochanek, C. S., Henning, Th., Gredel, R., Holoien, T. W. -. S., Rabus, M., Shappee, B. J., Billington, S. J., Campbell-White, J., and Zegmott, T. J. Fri .
"The 2014–2017 outburst of the young star ASASSN-13db: A time-resolved picture of a very-low-mass star between EXors and FUors*". United States. https://doi.org/10.1051/0004-6361/201731263. https://www.osti.gov/servlets/purl/1547046.
@article{osti_1547046,
title = {The 2014–2017 outburst of the young star ASASSN-13db: A time-resolved picture of a very-low-mass star between EXors and FUors*},
author = {Sicilia-Aguilar, A. and Oprandi, A. and Froebrich, D. and Fang, M. and Prieto, J. L. and Stanek, K. and Scholz, A. and Kochanek, C. S. and Henning, Th. and Gredel, R. and Holoien, T. W. -. S. and Rabus, M. and Shappee, B. J. and Billington, S. J. and Campbell-White, J. and Zegmott, T. J.},
abstractNote = {Context. Accretion outbursts are key elements in star formation. ASASSN-13db is a M5-type star with a protoplanetary disk, the lowest-mass star known to experience accretion outbursts. Since its discovery in 2013, it has experienced two outbursts, the second of which started in November 2014 and lasted until February 2017. Aims. We observe the photometric and spectroscopic behavior of ASASSN-13db during the 2014–2017 outburst. Methods. We use high- and low-resolution spectroscopy and time-resolved photometry from the ASAS-SN survey, the LCOGT and the Beacon Observatory to study the light curve of ASASSN-13db and the dynamical and physical properties of the accretion flow. Results. The 2014–2017 outburst lasted for nearly 800 days. A 4.15 d period in the light curve likely corresponds to rotational modulation of a star with hot spot(s). The spectra demonstrate multiple emission lines with variable inverse P-Cygni profiles and a highly variable blue-shifted absorption below the continuum. Line ratios from metallic emission lines (Fe I/Fe II, Ti I/Ti II) suggest temperatures of ~5800–6000 K in the accretion flow. Conclusions. Photometrically and spectroscopically, the 2014–2017 event displays an intermediate behavior between EXors and FUors. The accretion rate ([$\dot{M}$]= 1–3 × 10-7 M⊙/yr), about two orders of magnitude higher than the accretion rate in quiescence, is not vastly different from the accretion rate observed in 2013. The absorption features in the spectra suggest that the system is viewed at a high angle and drives a powerful, non-axisymmetric wind, maybe related to magnetic reconnection. The properties of ASASSN-13db suggest that temperatures lower than those for solar-type stars are needed for modeling accretion in very-low-mass systems. Finally, the rotational modulation during the outburst reveals that accretion-related structures settle after the beginning of the outburst and can be relatively stable and long-lived. Our work also demonstrates the power of time-resolved photometry and spectroscopy to explore the properties of variable and outbursting stars.},
doi = {10.1051/0004-6361/201731263},
journal = {Astronomy and Astrophysics},
number = ,
volume = 607,
place = {United States},
year = {Fri Nov 24 00:00:00 EST 2017},
month = {Fri Nov 24 00:00:00 EST 2017}
}
Web of Science
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