Toward a resolution of the bump and beat Cepheid mass discrepancies

Moskalik, P.; Buchler, J. R.; Marom, Ariel

doi:10.1086/170975

Cited by 144 publications

(119 citation statements)

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“…Below we briefly summarize the known resonances for Cepheids with periods P ≤ 10 d based on the work of Moskalik et al (1992) and Antonello (1994): a) There is a well known resonance F 2 /F 0 in Cepheids with P 0 near 10 d (see, for example, Moskalik et al 1992). For periods in the vicinity of 10 d , the primary and secondary bumps of the light curve switch roles, and as a result the bump appears to move from the descending to the ascending branch (Hertzsprung progression).…”

Section: Bumps Rotation and Resonancesmentioning

confidence: 99%

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Line profile variations in classical Cepheids

Kovtyukh

Andrievsky

Luck³

et al. 2003

A&A

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Abstract.We have investigated line profiles in a large sample of Cepheid spectra, and found four stars that show unusual (for Cepheids) line profile structure (bumps or/and asymmetries). The profiles can be phase dependent but the behavior persists over many cycles. The asymmetries are unlikely to be due to the spectroscopic binarity of these stars or the specific velocity field in their atmospheres caused by shock waves. As a preliminary hypothesis, we suggest that the observed features on the line profiles in the spectra of X Sgr, V1334 Cyg, EV Sct and BG Cru can be caused by the non-radial oscillations. It is possible that these non-radial oscillations are connected to resonances between the radial modes (3. d 2, 7. d 5 or 10. d 0).

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Section: Bumps Rotation and Resonancesmentioning

confidence: 99%

“…c) The resonance between the fundamental and fourth overtone mode F 3 /F 0 = 3 near P 0 = 7. d 5 has been studied by Moskalik et al (1992) in their non-linear calculations, and also discussed by Antonello (1994).…”

Section: Bumps Rotation and Resonancesmentioning

confidence: 99%

Line profile variations in classical Cepheids

Kovtyukh

Andrievsky

Luck³

et al. 2003

A&A

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“…Thus, the study of stellar pulsations provides indirect tests of opacities and has stimulated research. The "Z bump" is and important example, originally invoked to resolved mass discrepancies [26], soon after predicted by new opacity calculations [27,28], later corroborated by laboratory experiments [29] as well as pulsation studies [30], and now a standard feature in astrophysical opacities [31]. The Z bump is due to photon absorption by iron group elements.…”

Section: Stellar Envelope Opacitiesmentioning

confidence: 94%

Statistical line-by-line model for atomic spectra in intermediate coupling

Iglesias

2012

High Energy Density Physics

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The partially resolved transition array (PRTA) model is extended from JJ to intermediate coupling. The PRTA model conserves known array properties, yields improved higher moments, and systematically accounts for initial level populations. In addition, a random PRTA (R-PRTA) model is proposed to simulate detailed line accounting (DLA) calculations of complex spectra.Numerical examples show that the PRTA model with intermediate coupling reproduces the effects of the electrostatic interaction between spin-orbit split arrays on the spectrum. They also show that the R-PRTA model is in good agreement with DLA results and accounts for systematic line coincidences across transition arrays differing only in the subshell occupation of excited spectator electrons important in opacity calculations. Both PRTA and R-PRTA models are computationally much faster than DLA calculations. Hence, the models can accelerate spectrum calculations without introducing significant uncertainties whenever the DLA method is considered arduous or impractical.

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“…Cepheids in eclipsing binary systems are key objects for the determination of stellar masses and for the solution of the long-standing problem of Cepheid mass discrepancy (Christy 1968;Stobie 1969). This discrepancy was mainly resolved with new opacity tables (Moskalik et al 1992), but there is still a 17 ± 5% difference between the masses determined from the evolutionary models and the pulsation models (Keller 2008). The list of Cepheids belonging to eclipsing binaries in the Magellanic Clouds can be found in Szabados & Nehéz (2012).…”

Section: Introductionmentioning

confidence: 99%

Hunting for binary Cepheids using the “lucky imaging” technique

et al. 2013

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Detecting companions to Cepheids is difficult. In most cases the bright pulsator overshines the fainter secondary. Since Cepheids play a key role in determining the cosmic distance scale it is crucial to find binaries among the calibrating stars of the period-luminosity relation. Here we present an ongoing observing project of searching for faint and close companions of Galactic Cepheids using lucky imaging technique.

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Toward a resolution of the bump and beat Cepheid mass discrepancies

Cited by 144 publications

References 0 publications

Line profile variations in classical Cepheids

Line profile variations in classical Cepheids

Statistical line-by-line model for atomic spectra in intermediate coupling

Hunting for binary Cepheids using the “lucky imaging” technique

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