The origin of the diversity of type Ia supernovae and the environmental effects

Hideyuki Umeda, Ken'ichi Nomoto, Chiaki Kobayashi, Izumi Hachisu, Mariko Kato

Research output: Contribution to journalArticle

90 Citations (Scopus)

Abstract

Observations suggest that the properties of Type Ia supernovae (SNe Ia) may depend on environmental characteristics, such as the morphology, metallicity, and age of the host galaxies. The influence of these environmental properties on the resulting SNe Ia is studied in this Letter. First, it is shown that the carbon mass fraction X(C) in the C + O white dwarf SN Ia progenitors tends to be smaller for a lower metallicity environment and an older binary system. It is then suggested that the variation of X(C) causes the diversity in the brightness of SNe Ia: a smaller X(C) leads to a dimmer SN Ia. Further studies of the propagation of the turbulent flame are necessary to confirm this relation. Our model for the SN Ia progenitors then predicts that when the progenitors belong to an older population or to a low-metallicity environment, the number of bright SNe Ia is reduced, so that the variation in brightness among the SNe Ia is also smaller. Thus, our model can explain why the mean SN Ia brightness and its dispersion depend on the morphology of the host galaxies and on the distance of the SN from the center of the galaxy. It is further predicted that at higher redshift (z ≳ 1), both the mean brightness of SNe Ia and its variation should be smaller in spiral galaxies than in elliptical galaxies. These variations are within the range observed in nearby SNe Ia. Insofar as the variation in X(C) is the most important cause for the diversity among SNe Ia, the light-curve shape method that is currently used to determine the absolute magnitude of SNe Ia can also be applied to high-redshift SNe Ia.

Original languageEnglish
JournalAstrophysical Journal
Volume522
Issue number1 PART 2
Publication statusPublished - 1999 Sep 1

Fingerprint

environmental effect
supernovae
brightness
metallicity
galaxies
carbon
turbulent flames
causes
elliptical galaxies
spiral galaxies
light curve
propagation
method

Keywords

  • Binaries: Close
  • Cosmology: Miscellaneous
  • Stars: Evolution
  • Supernovae: General
  • White dwarfs

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Umeda, H., Nomoto, K., Kobayashi, C., Hachisu, I., & Kato, M. (1999). The origin of the diversity of type Ia supernovae and the environmental effects. Astrophysical Journal, 522(1 PART 2).

The origin of the diversity of type Ia supernovae and the environmental effects. / Umeda, Hideyuki; Nomoto, Ken'ichi; Kobayashi, Chiaki; Hachisu, Izumi; Kato, Mariko.

In: Astrophysical Journal, Vol. 522, No. 1 PART 2, 01.09.1999.

Research output: Contribution to journalArticle

Umeda, H, Nomoto, K, Kobayashi, C, Hachisu, I & Kato, M 1999, 'The origin of the diversity of type Ia supernovae and the environmental effects', Astrophysical Journal, vol. 522, no. 1 PART 2.
Umeda H, Nomoto K, Kobayashi C, Hachisu I, Kato M. The origin of the diversity of type Ia supernovae and the environmental effects. Astrophysical Journal. 1999 Sep 1;522(1 PART 2).
Umeda, Hideyuki ; Nomoto, Ken'ichi ; Kobayashi, Chiaki ; Hachisu, Izumi ; Kato, Mariko. / The origin of the diversity of type Ia supernovae and the environmental effects. In: Astrophysical Journal. 1999 ; Vol. 522, No. 1 PART 2.
@article{0cffce50af05445f9303bdf73d32c7ae,
title = "The origin of the diversity of type Ia supernovae and the environmental effects",
abstract = "Observations suggest that the properties of Type Ia supernovae (SNe Ia) may depend on environmental characteristics, such as the morphology, metallicity, and age of the host galaxies. The influence of these environmental properties on the resulting SNe Ia is studied in this Letter. First, it is shown that the carbon mass fraction X(C) in the C + O white dwarf SN Ia progenitors tends to be smaller for a lower metallicity environment and an older binary system. It is then suggested that the variation of X(C) causes the diversity in the brightness of SNe Ia: a smaller X(C) leads to a dimmer SN Ia. Further studies of the propagation of the turbulent flame are necessary to confirm this relation. Our model for the SN Ia progenitors then predicts that when the progenitors belong to an older population or to a low-metallicity environment, the number of bright SNe Ia is reduced, so that the variation in brightness among the SNe Ia is also smaller. Thus, our model can explain why the mean SN Ia brightness and its dispersion depend on the morphology of the host galaxies and on the distance of the SN from the center of the galaxy. It is further predicted that at higher redshift (z ≳ 1), both the mean brightness of SNe Ia and its variation should be smaller in spiral galaxies than in elliptical galaxies. These variations are within the range observed in nearby SNe Ia. Insofar as the variation in X(C) is the most important cause for the diversity among SNe Ia, the light-curve shape method that is currently used to determine the absolute magnitude of SNe Ia can also be applied to high-redshift SNe Ia.",
keywords = "Binaries: Close, Cosmology: Miscellaneous, Stars: Evolution, Supernovae: General, White dwarfs",
author = "Hideyuki Umeda and Ken'ichi Nomoto and Chiaki Kobayashi and Izumi Hachisu and Mariko Kato",
year = "1999",
month = "9",
day = "1",
language = "English",
volume = "522",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "1 PART 2",

}

TY - JOUR

T1 - The origin of the diversity of type Ia supernovae and the environmental effects

AU - Umeda, Hideyuki

AU - Nomoto, Ken'ichi

AU - Kobayashi, Chiaki

AU - Hachisu, Izumi

AU - Kato, Mariko

PY - 1999/9/1

Y1 - 1999/9/1

N2 - Observations suggest that the properties of Type Ia supernovae (SNe Ia) may depend on environmental characteristics, such as the morphology, metallicity, and age of the host galaxies. The influence of these environmental properties on the resulting SNe Ia is studied in this Letter. First, it is shown that the carbon mass fraction X(C) in the C + O white dwarf SN Ia progenitors tends to be smaller for a lower metallicity environment and an older binary system. It is then suggested that the variation of X(C) causes the diversity in the brightness of SNe Ia: a smaller X(C) leads to a dimmer SN Ia. Further studies of the propagation of the turbulent flame are necessary to confirm this relation. Our model for the SN Ia progenitors then predicts that when the progenitors belong to an older population or to a low-metallicity environment, the number of bright SNe Ia is reduced, so that the variation in brightness among the SNe Ia is also smaller. Thus, our model can explain why the mean SN Ia brightness and its dispersion depend on the morphology of the host galaxies and on the distance of the SN from the center of the galaxy. It is further predicted that at higher redshift (z ≳ 1), both the mean brightness of SNe Ia and its variation should be smaller in spiral galaxies than in elliptical galaxies. These variations are within the range observed in nearby SNe Ia. Insofar as the variation in X(C) is the most important cause for the diversity among SNe Ia, the light-curve shape method that is currently used to determine the absolute magnitude of SNe Ia can also be applied to high-redshift SNe Ia.

AB - Observations suggest that the properties of Type Ia supernovae (SNe Ia) may depend on environmental characteristics, such as the morphology, metallicity, and age of the host galaxies. The influence of these environmental properties on the resulting SNe Ia is studied in this Letter. First, it is shown that the carbon mass fraction X(C) in the C + O white dwarf SN Ia progenitors tends to be smaller for a lower metallicity environment and an older binary system. It is then suggested that the variation of X(C) causes the diversity in the brightness of SNe Ia: a smaller X(C) leads to a dimmer SN Ia. Further studies of the propagation of the turbulent flame are necessary to confirm this relation. Our model for the SN Ia progenitors then predicts that when the progenitors belong to an older population or to a low-metallicity environment, the number of bright SNe Ia is reduced, so that the variation in brightness among the SNe Ia is also smaller. Thus, our model can explain why the mean SN Ia brightness and its dispersion depend on the morphology of the host galaxies and on the distance of the SN from the center of the galaxy. It is further predicted that at higher redshift (z ≳ 1), both the mean brightness of SNe Ia and its variation should be smaller in spiral galaxies than in elliptical galaxies. These variations are within the range observed in nearby SNe Ia. Insofar as the variation in X(C) is the most important cause for the diversity among SNe Ia, the light-curve shape method that is currently used to determine the absolute magnitude of SNe Ia can also be applied to high-redshift SNe Ia.

KW - Binaries: Close

KW - Cosmology: Miscellaneous

KW - Stars: Evolution

KW - Supernovae: General

KW - White dwarfs

UR - http://www.scopus.com/inward/record.url?scp=0033193536&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=0033193536&partnerID=8YFLogxK

M3 - Article

AN - SCOPUS:0033193536

VL - 522

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1 PART 2

ER -