Spectra of Type II Cepheids
نویسندگان
چکیده
منابع مشابه
Period-Luminosity Relation for Type II Cepheids
We have estimated JHKs magnitudes corrected to mean intensity for LMC type II Cepheids found in the OGLE-III survey. Period-luminosity relations (PLRs) are derived in JHKs as well as in a reddening-free V I parameter. The BL Her stars (P < 4 d) and the W Vir stars (P = 4 to 20 d) are co-linear in these PLRs. The slopes of the infrared relations agree with those found previously for type II Ceph...
متن کاملPeriod-Luminosity Relations for Type II Cepheids and their Application
JHKs magnitudes corrected to mean intensity are estimated for LMC type II Cepheids in the OGLE-III survey. Period-luminosity (PL) relations are derived in JHKs as well as in a reddening-free V I parameter. Within the uncertainties the BL Her stars (P < 4 d) and the W Vir stars (P = 4 to 20 d) are co-linear in these PL relations. The slopes of the infrared relations agree with those found previo...
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Photometric data for 593 Cepheids in the LMC, measured by Udalski et al. in the OGLE survey, augmented by 92 longer period Cepheids from other sources, are analyzed for the period-color (P-C) and period-luminosity (P-L) relations, and for the variations of amplitude, light curve shape, and period across the instability strip at constant absolute magnitude. Both the P-C and P-L relations have di...
متن کاملEvolutionary scenario for metal-poor pulsating stars I. Type II Cepheids
Pulsating convective models and evolutionary tracks are used to constrainmass, luminosity, and effective temperature of metal-poor (Z in the range of 0.0001 to 0.001) low-mass (0.52M –0.80M ) fundamental pulsators connected with the horizontal branch and asymptotic branch phase. On this basis the fundamental period P (F ) and the absolute blue magnitudeB of the pulsators are calculated. We show...
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Nonlinear, radiative models for long–period Cepheids in the Magellanic Clouds were constructed and the theoretical light and velocity curves were compared with observations. We assumed a metal content Z = 0.005, and two mass–luminosity M–L relations: one was obtained from stellar evolution calculation with convective overshooting models, and the other, which gives an even larger L for the same ...
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ژورنال
عنوان ژورنال: Symposium - International Astronomical Union
سال: 1975
ISSN: 0074-1809
DOI: 10.1017/s0074180900010779