SN 2009ip: CONSTRAINTS ON THE PROGENITOR MASS-LOSS RATE
Abstract
Some supernovae (SNe) show evidence for mass-loss events taking place prior to their explosions. Measuring their pre-outburst mass-loss rates provides essential information regarding the mechanisms that are responsible for these events. Here we present XMM-Newton and Swift X-ray observations taken after the latest, and presumably the final, outburst of SN 2009ip. We use these observations as well as new near-infrared and visible-light spectra and published radio and visible-light observations to put six independent order-of-magnitude constraints on the mass-loss rate of the SN progenitor prior to the explosion. Our methods utilize the X-ray luminosity, the bound-free absorption, the H{alpha} luminosity, the SN rise time, free-free absorption, and the bolometric luminosity of the outburst detected prior to the explosion. Assuming spherical mass loss with a wind-density profile, we estimate that the effective mass-loss rate from the progenitor was between 10{sup -3} and 10{sup -2} M{sub Sun} yr{sup -1}, over a few years prior to the explosion, with a velocity of {approx}10{sup 3} km s{sup -1}. This mass-loss rate corresponds to a total circumstellar matter (CSM) mass of {approx}0.04 M{sub Sun }, within 6 Multiplication-Sign 10{sup 15} cm of the SN. We note that the mass-loss rate estimate based on the H{alpha} luminositymore »
- Authors:
-
- Benoziyo Center for Astrophysics and the Helen Kimmel Center for Planetary Science, Weizmann Institute of Science, 76100 Rehovot (Israel)
- Faculty of Engineering and Natural Sciences, Sabanc Latin-Small-Letter-Dotless-I University, Orhanl Latin-Small-Letter-Dotless-I -Tuzla, Istanbul 34956 (Turkey)
- Space Science Office, ZP-12, NASA/Marshall Space Flight Center, Huntsville, AL 35812 (United States)
- Universities Space Research Association, 6767 Old Madison Pike NW, Suite 450, Huntsville, AL 35806 (United States)
- Observatories of the Carnegie Institution for Science, 813 Santa Barbara St, Pasadena, CA 91101 (United States)
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125 (United States)
- Publication Date:
- OSTI Identifier:
- 22126837
- Resource Type:
- Journal Article
- Journal Name:
- Astrophysical Journal
- Additional Journal Information:
- Journal Volume: 768; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ABSORPTION; DENSITY; EFFECTIVE MASS; EXPLOSIONS; LOSSES; LUMINOSITY; MASS TRANSFER; MATTER; SPECTRA; STELLAR WINDS; SUPERNOVAE; VELOCITY; X RADIATION
Citation Formats
Ofek, E. O., Lin, L., Goegues, E., Kouveliotou, C., Younes, G., Kasliwal, M. M., and Cao, Y. SN 2009ip: CONSTRAINTS ON THE PROGENITOR MASS-LOSS RATE. United States: N. p., 2013.
Web. doi:10.1088/0004-637X/768/1/47.
Ofek, E. O., Lin, L., Goegues, E., Kouveliotou, C., Younes, G., Kasliwal, M. M., & Cao, Y. SN 2009ip: CONSTRAINTS ON THE PROGENITOR MASS-LOSS RATE. United States. https://doi.org/10.1088/0004-637X/768/1/47
Ofek, E. O., Lin, L., Goegues, E., Kouveliotou, C., Younes, G., Kasliwal, M. M., and Cao, Y. 2013.
"SN 2009ip: CONSTRAINTS ON THE PROGENITOR MASS-LOSS RATE". United States. https://doi.org/10.1088/0004-637X/768/1/47.
@article{osti_22126837,
title = {SN 2009ip: CONSTRAINTS ON THE PROGENITOR MASS-LOSS RATE},
author = {Ofek, E. O. and Lin, L. and Goegues, E. and Kouveliotou, C. and Younes, G. and Kasliwal, M. M. and Cao, Y.},
abstractNote = {Some supernovae (SNe) show evidence for mass-loss events taking place prior to their explosions. Measuring their pre-outburst mass-loss rates provides essential information regarding the mechanisms that are responsible for these events. Here we present XMM-Newton and Swift X-ray observations taken after the latest, and presumably the final, outburst of SN 2009ip. We use these observations as well as new near-infrared and visible-light spectra and published radio and visible-light observations to put six independent order-of-magnitude constraints on the mass-loss rate of the SN progenitor prior to the explosion. Our methods utilize the X-ray luminosity, the bound-free absorption, the H{alpha} luminosity, the SN rise time, free-free absorption, and the bolometric luminosity of the outburst detected prior to the explosion. Assuming spherical mass loss with a wind-density profile, we estimate that the effective mass-loss rate from the progenitor was between 10{sup -3} and 10{sup -2} M{sub Sun} yr{sup -1}, over a few years prior to the explosion, with a velocity of {approx}10{sup 3} km s{sup -1}. This mass-loss rate corresponds to a total circumstellar matter (CSM) mass of {approx}0.04 M{sub Sun }, within 6 Multiplication-Sign 10{sup 15} cm of the SN. We note that the mass-loss rate estimate based on the H{alpha} luminosity is higher by an order of magnitude. This can be explained if the narrow-line H{alpha} component is generated at radii larger than the shock radius, or if the CSM has an aspherical geometry. We discuss simple geometries which are consistent with our results.},
doi = {10.1088/0004-637X/768/1/47},
url = {https://www.osti.gov/biblio/22126837},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 1,
volume = 768,
place = {United States},
year = {Wed May 01 00:00:00 EDT 2013},
month = {Wed May 01 00:00:00 EDT 2013}
}