Light-curve models for supernova SN1987A in the Large Magellanic Cloud

T. Shigeyama, K. Nomoto, Masa-Aki Hashimoto, D. Sugimoto

Research output: Contribution to journalArticle

33 Citations (Scopus)

Abstract

Neutrino bursts from the supernova SN1987A have been reported1-3 which provide qualitatively new information as to the time interval between the core collapse and the optical flaring of the supernova up to about 6 mag 4. The interval that we take as three hours1,2 imposes conditions on the radius of the progenitor star and the energetics of the explosion. As for the brightness and its time change, the relatively less bright visual magnitude at the plateau in the light curve during the initial eight days or so (refs 5, 29) as well. The subsequent light curve after eight days is quite unique; the bolometric luminosity increases until ∼65 days (ref. 29) but thereafter it seems to level off gradually (J. Walsh and R. Stathakis, personal communication; M.A. Dopita, personal communication). To maintain the bolometric luminosity of the star means that certain conditions should be imposed on the energy source. By computing the propagation of shock wave, the subsequent expansion of ejected matter and the optical light curve, we find that the early light curve can be accounted for by the diffusive release of energy deposited by the shock wave, that the progenitor's radius should be as small as ∼(1-3) × 1012 cm, and that the explosion energy per unit mass should be relatively large, ∼(2-3)× 1051 erg for the ejected matter of 7-10 M. The light curve after eight days is well reproduced by using a model with constant energy input. The energy input may be due to the activity of an embedded pulsar. The light curves calculated by invoking the radioactive decay of 56Ni and 56Co are less satisfactory in accounting for the nearly flat portion observed after 65 days. Supposing Sk-69 202 is the progenitor of SN1987A13,14, its explosion energy should be >2×l051erg; this suggests that a prompt shock mechanism forms a neutron star.

Original languageEnglish
Pages (from-to)320-323
Number of pages4
JournalNature
Volume328
Issue number6128
Publication statusPublished - Dec 1 1988

Fingerprint

Magellanic clouds
light curve
supernovae
explosions
shock waves
communication
luminosity
energy
intervals
stars
radioactive decay
radii
energy sources
pulsars
neutron stars
plateaus
bursts
brightness
neutrinos
shock

All Science Journal Classification (ASJC) codes

  • General

Cite this

Shigeyama, T., Nomoto, K., Hashimoto, M-A., & Sugimoto, D. (1988). Light-curve models for supernova SN1987A in the Large Magellanic Cloud. Nature, 328(6128), 320-323.

Light-curve models for supernova SN1987A in the Large Magellanic Cloud. / Shigeyama, T.; Nomoto, K.; Hashimoto, Masa-Aki; Sugimoto, D.

In: Nature, Vol. 328, No. 6128, 01.12.1988, p. 320-323.

Research output: Contribution to journalArticle

Shigeyama, T, Nomoto, K, Hashimoto, M-A & Sugimoto, D 1988, 'Light-curve models for supernova SN1987A in the Large Magellanic Cloud', Nature, vol. 328, no. 6128, pp. 320-323.
Shigeyama T, Nomoto K, Hashimoto M-A, Sugimoto D. Light-curve models for supernova SN1987A in the Large Magellanic Cloud. Nature. 1988 Dec 1;328(6128):320-323.
Shigeyama, T. ; Nomoto, K. ; Hashimoto, Masa-Aki ; Sugimoto, D. / Light-curve models for supernova SN1987A in the Large Magellanic Cloud. In: Nature. 1988 ; Vol. 328, No. 6128. pp. 320-323.
@article{916a75f0bb7d47609e3b3c253cb0f6a6,
title = "Light-curve models for supernova SN1987A in the Large Magellanic Cloud",
abstract = "Neutrino bursts from the supernova SN1987A have been reported1-3 which provide qualitatively new information as to the time interval between the core collapse and the optical flaring of the supernova up to about 6 mag 4. The interval that we take as three hours1,2 imposes conditions on the radius of the progenitor star and the energetics of the explosion. As for the brightness and its time change, the relatively less bright visual magnitude at the plateau in the light curve during the initial eight days or so (refs 5, 29) as well. The subsequent light curve after eight days is quite unique; the bolometric luminosity increases until ∼65 days (ref. 29) but thereafter it seems to level off gradually (J. Walsh and R. Stathakis, personal communication; M.A. Dopita, personal communication). To maintain the bolometric luminosity of the star means that certain conditions should be imposed on the energy source. By computing the propagation of shock wave, the subsequent expansion of ejected matter and the optical light curve, we find that the early light curve can be accounted for by the diffusive release of energy deposited by the shock wave, that the progenitor's radius should be as small as ∼(1-3) × 1012 cm, and that the explosion energy per unit mass should be relatively large, ∼(2-3)× 1051 erg for the ejected matter of 7-10 M⊙. The light curve after eight days is well reproduced by using a model with constant energy input. The energy input may be due to the activity of an embedded pulsar. The light curves calculated by invoking the radioactive decay of 56Ni and 56Co are less satisfactory in accounting for the nearly flat portion observed after 65 days. Supposing Sk-69 202 is the progenitor of SN1987A13,14, its explosion energy should be >2×l051erg; this suggests that a prompt shock mechanism forms a neutron star.",
author = "T. Shigeyama and K. Nomoto and Masa-Aki Hashimoto and D. Sugimoto",
year = "1988",
month = "12",
day = "1",
language = "English",
volume = "328",
pages = "320--323",
journal = "Nature",
issn = "0028-0836",
publisher = "Nature Publishing Group",
number = "6128",

}

TY - JOUR

T1 - Light-curve models for supernova SN1987A in the Large Magellanic Cloud

AU - Shigeyama, T.

AU - Nomoto, K.

AU - Hashimoto, Masa-Aki

AU - Sugimoto, D.

PY - 1988/12/1

Y1 - 1988/12/1

N2 - Neutrino bursts from the supernova SN1987A have been reported1-3 which provide qualitatively new information as to the time interval between the core collapse and the optical flaring of the supernova up to about 6 mag 4. The interval that we take as three hours1,2 imposes conditions on the radius of the progenitor star and the energetics of the explosion. As for the brightness and its time change, the relatively less bright visual magnitude at the plateau in the light curve during the initial eight days or so (refs 5, 29) as well. The subsequent light curve after eight days is quite unique; the bolometric luminosity increases until ∼65 days (ref. 29) but thereafter it seems to level off gradually (J. Walsh and R. Stathakis, personal communication; M.A. Dopita, personal communication). To maintain the bolometric luminosity of the star means that certain conditions should be imposed on the energy source. By computing the propagation of shock wave, the subsequent expansion of ejected matter and the optical light curve, we find that the early light curve can be accounted for by the diffusive release of energy deposited by the shock wave, that the progenitor's radius should be as small as ∼(1-3) × 1012 cm, and that the explosion energy per unit mass should be relatively large, ∼(2-3)× 1051 erg for the ejected matter of 7-10 M⊙. The light curve after eight days is well reproduced by using a model with constant energy input. The energy input may be due to the activity of an embedded pulsar. The light curves calculated by invoking the radioactive decay of 56Ni and 56Co are less satisfactory in accounting for the nearly flat portion observed after 65 days. Supposing Sk-69 202 is the progenitor of SN1987A13,14, its explosion energy should be >2×l051erg; this suggests that a prompt shock mechanism forms a neutron star.

AB - Neutrino bursts from the supernova SN1987A have been reported1-3 which provide qualitatively new information as to the time interval between the core collapse and the optical flaring of the supernova up to about 6 mag 4. The interval that we take as three hours1,2 imposes conditions on the radius of the progenitor star and the energetics of the explosion. As for the brightness and its time change, the relatively less bright visual magnitude at the plateau in the light curve during the initial eight days or so (refs 5, 29) as well. The subsequent light curve after eight days is quite unique; the bolometric luminosity increases until ∼65 days (ref. 29) but thereafter it seems to level off gradually (J. Walsh and R. Stathakis, personal communication; M.A. Dopita, personal communication). To maintain the bolometric luminosity of the star means that certain conditions should be imposed on the energy source. By computing the propagation of shock wave, the subsequent expansion of ejected matter and the optical light curve, we find that the early light curve can be accounted for by the diffusive release of energy deposited by the shock wave, that the progenitor's radius should be as small as ∼(1-3) × 1012 cm, and that the explosion energy per unit mass should be relatively large, ∼(2-3)× 1051 erg for the ejected matter of 7-10 M⊙. The light curve after eight days is well reproduced by using a model with constant energy input. The energy input may be due to the activity of an embedded pulsar. The light curves calculated by invoking the radioactive decay of 56Ni and 56Co are less satisfactory in accounting for the nearly flat portion observed after 65 days. Supposing Sk-69 202 is the progenitor of SN1987A13,14, its explosion energy should be >2×l051erg; this suggests that a prompt shock mechanism forms a neutron star.

UR - http://www.scopus.com/inward/record.url?scp=0000797462&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=0000797462&partnerID=8YFLogxK

M3 - Article

AN - SCOPUS:0000797462

VL - 328

SP - 320

EP - 323

JO - Nature

JF - Nature

SN - 0028-0836

IS - 6128

ER -