Nonlinear models of the bump cepheid HV 905 and the distance modulus to the large magellanic cloud

P R Wood, A S Arnold, K M Sebo

Research output: Contribution to journalArticle

32 Citations (Scopus)

Abstract

Nonlinear pulsation models have been used to simulate the light curve of the LMC bump Cepheid HV 905. In order to reproduce the light curve accurately, tight constraints on the input parameters M, L, and T-eff are required. The results, combined with accurate existing V and I photometry, yield an LMC distance modulus of 18.51 +/- 0.05, and they show that the luminosity of HV 905 is much higher than expected from the mass-luminosity relation of stellar evolution theory. If we assume that the pulsation models are accurate, this suggests that there is a larger amount of convective core overshoot during the main-sequence evolution of stars with M similar to 5 M. than is usually assumed.

LanguageEnglish
PagesL25-L28
Number of pages4
JournalAstrophysical Journal
Volume485
Issue number1
DOIs
Publication statusPublished - 10 Aug 1997

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Magellanic clouds
light curve
luminosity
stellar evolution
photometry
stars
parameter

Keywords

  • stars, oscillations
  • cepheids
  • magellanic clouds
  • pulsation
  • masses
  • stars
  • opacities
  • nonlinear models
  • bump cepheid
  • hv 905
  • distance modulus

Cite this

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title = "Nonlinear models of the bump cepheid HV 905 and the distance modulus to the large magellanic cloud",
abstract = "Nonlinear pulsation models have been used to simulate the light curve of the LMC bump Cepheid HV 905. In order to reproduce the light curve accurately, tight constraints on the input parameters M, L, and T-eff are required. The results, combined with accurate existing V and I photometry, yield an LMC distance modulus of 18.51 +/- 0.05, and they show that the luminosity of HV 905 is much higher than expected from the mass-luminosity relation of stellar evolution theory. If we assume that the pulsation models are accurate, this suggests that there is a larger amount of convective core overshoot during the main-sequence evolution of stars with M similar to 5 M. than is usually assumed.",
keywords = "stars, oscillations, cepheids, magellanic clouds, pulsation, masses, stars , opacities, nonlinear models, bump cepheid, hv 905, distance modulus",
author = "Wood, {P R} and Arnold, {A S} and Sebo, {K M}",
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Nonlinear models of the bump cepheid HV 905 and the distance modulus to the large magellanic cloud. / Wood, P R ; Arnold, A S ; Sebo, K M .

In: Astrophysical Journal, Vol. 485, No. 1, 10.08.1997, p. L25-L28.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Nonlinear models of the bump cepheid HV 905 and the distance modulus to the large magellanic cloud

AU - Wood, P R

AU - Arnold, A S

AU - Sebo, K M

PY - 1997/8/10

Y1 - 1997/8/10

N2 - Nonlinear pulsation models have been used to simulate the light curve of the LMC bump Cepheid HV 905. In order to reproduce the light curve accurately, tight constraints on the input parameters M, L, and T-eff are required. The results, combined with accurate existing V and I photometry, yield an LMC distance modulus of 18.51 +/- 0.05, and they show that the luminosity of HV 905 is much higher than expected from the mass-luminosity relation of stellar evolution theory. If we assume that the pulsation models are accurate, this suggests that there is a larger amount of convective core overshoot during the main-sequence evolution of stars with M similar to 5 M. than is usually assumed.

AB - Nonlinear pulsation models have been used to simulate the light curve of the LMC bump Cepheid HV 905. In order to reproduce the light curve accurately, tight constraints on the input parameters M, L, and T-eff are required. The results, combined with accurate existing V and I photometry, yield an LMC distance modulus of 18.51 +/- 0.05, and they show that the luminosity of HV 905 is much higher than expected from the mass-luminosity relation of stellar evolution theory. If we assume that the pulsation models are accurate, this suggests that there is a larger amount of convective core overshoot during the main-sequence evolution of stars with M similar to 5 M. than is usually assumed.

KW - stars, oscillations

KW - cepheids

KW - magellanic clouds

KW - pulsation

KW - masses

KW - stars

KW - opacities

KW - nonlinear models

KW - bump cepheid

KW - hv 905

KW - distance modulus

U2 - 10.1086/310798

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