PROBING FINAL STAGES OF STELLAR EVOLUTION WITH X-RAY OBSERVATIONS OF SN 2013ej

被引:29
作者
Chakraborti, Sayan [1 ,11 ]
Ray, Alak [1 ,12 ]
Smith, Randall [2 ]
Margutti, Raffaella [3 ]
Pooley, David [4 ]
Bose, Subhash [5 ]
Sutaria, Firoza [6 ]
Chandra, Poonam [7 ]
Dwarkadas, Vikram V. [8 ]
Ryder, Stuart [9 ]
Maeda, Keiichi [10 ]
机构
[1] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA
[2] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA
[3] NYU, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA
[4] Trinity Univ, Dept Phys & Astron, San Antonio, TX 78212 USA
[5] Aryabhatta Res Inst Observat Sci, Manora Peak, Nainital, India
[6] Indian Inst Astrophys, Bangalore 560034, Karnataka, India
[7] Natl Ctr Radio Astrophys, Pune Univ Campus, Pune 411007, Maharashtra, India
[8] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA
[9] Australian Astron Observ, POB 915, N Ryde, NSW 1670, Australia
[10] Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan
[11] Harvard Univ, 78 Mt Auburn St, Cambridge, MA 02138 USA
[12] Tata Inst Fundamental Res, 1 Homi Bhabha Rd, Bombay 400005, Maharashtra, India
基金
美国国家航空航天局;
关键词
circumstellar matter; shock waves; stars: mass-loss; supernovae: individual (SN 2013ej); X-rays: general; SUPERNOVA-REMNANTS; MASS-LOSS; IIL SUPERNOVA; LIGHT CURVES; EMISSION; STARS; PROGENITOR; SHOCKS; 2009IP; M74;
D O I
10.3847/0004-637X/817/1/22
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Massive stars shape their surroundings with mass loss from winds during their lifetimes. Fast ejecta from supernovae (SNe), from these massive stars, shock this circumstellar medium. Emission generated by this interaction provides a window into the final stages of stellar evolution, by probing the history of mass loss from the progenitor. Here we use Chandra and Swift. X-ray observations of the type II-P/L SN 2013ej to probe the history of mass loss from its progenitor. We model the observed X-rays as emission from both heated circumstellar matter and SN ejecta. The circumstellar density profile probed by the SN shock reveals a history of steady mass loss during the final 400 years. The inferred mass loss rate of 3 '10-6M(circle dot) yr(-1). points back to a 14 M-circle dot progenitor. Soon after the explosion we find significant absorption of reverse shock emission by a cooling shell. The column depth of this shell observed in absorption provides an independent and consistent measurement of the circumstellar density seen in emission. We also determine the efficiency of cosmic ray acceleration from X-rays produced by Inverse Compton scattering of optical photons by relativistic electrons. Only about 1% of the thermal energy is used to accelerate electrons. Our X-ray observations and modeling provide stringent tests for models of massive stellar evolution and micro-physics of shocks.
引用
收藏
页数:8
相关论文
共 54 条
  • [1] Andrews J. E., 2015, ARXIV150906379
  • [2] Arnaud K. A., 2013, AAS HIGH ENERGY ASTR, V13
  • [3] The Chemical Composition of the Sun
    Asplund, Martin
    Grevesse, Nicolas
    Sauval, A. Jacques
    Scott, Pat
    [J]. ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS, VOL 47, 2009, 47 : 481 - 522
  • [4] MAGNETOHYDRODYNAMIC-PARTICLE-IN-CELL METHOD FOR COUPLING COSMIC RAYS WITH A THERMAL PLASMA: APPLICATION TO NON-RELATIVISTIC SHOCKS
    Bai, Xue-Ning
    Caprioli, Damiano
    Sironi, Lorenzo
    Spitkovsky, Anatoly
    [J]. ASTROPHYSICAL JOURNAL, 2015, 809 (01)
  • [5] BOLOMETRIC LIGHT CURVES FOR 33 TYPE II PLATEAU SUPERNOVAE
    Bersten, Melina C.
    Hamuy, Mario
    [J]. ASTROPHYSICAL JOURNAL, 2009, 701 (01) : 200 - 208
  • [6] SN 2013ej: A TYPE IIL SUPERNOVA WITH WEAK SIGNS OF INTERACTION
    Bose, Subhash
    Sutaria, Firoza
    Kumar, Brijesh
    Duggal, Chetna
    Misra, Kuntal
    Brown, Peter J.
    Singh, Mridweeka
    Dwarkadas, Vikram
    York, Donald G.
    Chakraborti, Sayan
    Chandola, H. C.
    Dahlstrom, Julie
    Ray, Alak
    Safonova, Margarita
    [J]. ASTROPHYSICAL JOURNAL, 2015, 806 (02)
  • [7] CASH W, 1979, ASTROPHYS J, V228, P939, DOI 10.1086/156922
  • [8] Two-dimensional metallicity distribution of the ionized gas in NGC 628 and NGC 6946
    Cedres, B.
    Cepa, J.
    Bongiovanni, A.
    Castaneda, H.
    Sanchez-Portal, M.
    Tomita, A.
    [J]. ASTRONOMY & ASTROPHYSICS, 2012, 545
  • [9] THE PROGENITOR OF SN 2011ja: CLUES FROM CIRCUMSTELLAR INTERACTION
    Chakraborti, Sayan
    Ray, Alak
    Smith, Randall
    Ryder, Stuart
    Yadav, Naveen
    Sutaria, Firoza
    Dwarkadas, Vikram V.
    Chandra, Poonam
    Pooley, David
    Roy, Rupak
    [J]. ASTROPHYSICAL JOURNAL, 2013, 774 (01)
  • [10] X-RAY EMISSION FROM SN 2004dj: A TALE OF TWO SHOCKS
    Chakraborti, Sayan
    Yadav, Naveen
    Ray, Alak
    Smith, Randall
    Chandra, Poonam
    Pooley, David
    [J]. ASTROPHYSICAL JOURNAL, 2012, 761 (02)