HD 99458: First time ever Ap-type star as a δ Scuti pulsator in a short period eclipsing binary?

Skarka, Marek; Kabáth, P.; Paunzen, E.; Fedurco, M.; Budaj, J.; Dupkala, Daniel; Krtička, Jiřı́; Hatzes, A. P.; Pribulla, T.; Parimucha, Š.; Mikulášek, Zdeněk; Guenther, E. W.; Sabotta, S.; Blažek, Martin; Dvořáková, J.; Hambálek, Ľ.; Klocová, T.; Kollár, Vojtech; Kundra, E.; Šlechta, M.; Vaňko, M.

doi:10.1093/mnras/stz1478

Cited by 22 publications

(21 citation statements)

References 41 publications

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“…In summary, we conclude that at least one component of the LAMOST J034306.74+495240.7 system is a Si CP2 star. It is, therefore, of great interest because mCP stars in eclipsing binaries are exceedingly rare (Renson & Manfroid 2009;Niemczura et al 2017;Kochukhov et al 2018;Skarka et al 2019) and accurate parameters for the components can be derived via an orbital solution of the system. We strongly encourage further studies of this interesting object.…”

Section: The Eclipsing Binary Systemmentioning

confidence: 99%

A plethora of new, magnetic chemically peculiar stars from LAMOST DR4

Hümmerich

Paunzen

Bernhard

2020

A&A

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Context. Magnetic chemically peculiar (mCP) stars are important to astrophysics because their complex atmospheres lend themselves perfectly to the investigation of the interplay between such diverse phenomena as atomic diffusion, magnetic fields, and stellar rotation. The most up-to-date catalogue of these objects was published a decade ago. Since then, no large scale spectroscopic surveys targeting this group of objects have been carried out. An increased sample size of mCP stars, however, is important for statistical studies. Aims. The present work is aimed at identifying new mCP stars using spectra collected by the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST). Methods. Suitable candidates were selected by searching LAMOST DR4 spectra for the presence of the characteristic 5200 Å flux depression. Spectral classification was carried out with a modified version of the MKCLASS code and the accuracy of the classifications was estimated by comparison with results from manual classification and the literature. Using parallax data and photometry from Gaia DR2, we investigated the space distribution of our sample stars and their properties in the colour-magnitude diagram. Results. Our final sample consists of 1002 mCP stars, most of which are new discoveries (only 59 common entries with the Catalogue of Ap, HgMn and Am stars). Traditional mCP star peculiarities have been identified in all but 36 stars, highlighting the efficiency of the code’s peculiarity identification capabilities. The derived temperature and peculiarity types are in agreement with manually derived classifications and the literature. Our sample stars are between 100 Myr and 1 Gyr old, with the majority having masses between 2 M⊙ and 3 M⊙. Our results could be considered as strong evidence for an inhomogeneous age distribution among low-mass (M < 3 M⊙) mCP stars; however, we caution that our sample has not been selected on the basis of an unbiased, direct detection of a magnetic field. We identified several astrophysically interesting objects: the mCP stars LAMOST J122746.05+113635.3 and LAMOST J150331.87+093125.4 have distances and kinematical properties in agreement with halo stars; LAMOST J034306.74+495240.7 is an eclipsing binary system (Porb = 5.1435 ± 0.0012 d) hosting an mCP star component; and LAMOST J050146.85+383500.8 was found to be an SB2 system likely comprising of an mCP star and a supergiant component. Conclusions. With our work, we significantly increase the sample size of known Galactic mCP stars, paving the way for future in-depth statistical studies.

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Section: The Eclipsing Binary Systemmentioning

confidence: 99%

A plethora of new, magnetic chemically peculiar stars from LAMOST DR4

Hümmerich

Paunzen

Bernhard

2020

A&A

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“…Skarka et al [57] reported the very first discovery of a pulsating Ap star in the EB HD 99458. The binary system consists of a chemically peculiar (CP) Ap-type star exhibiting δ Sct pulsations and a low-mass early-M type dwarf star that are on an inclined orbit with an orbital period of 2.722 d and grazing eclipses.…”

Section: Resultsmentioning

confidence: 99%

Eclipsing Systems with Pulsating Components (Types β Cep, δ Sct, γ Dor or Red Giant) in the Era of High-Accuracy Space Data

Lampens

2021

Galaxies

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Eclipsing systems are essential objects for understanding the properties of stars and stellar systems. Eclipsing systems with pulsating components are furthermore advantageous because they provide accurate constraints on the component properties, as well as a complementary method for pulsation mode determination, crucial for precise asteroseismology. The outcome of space missions aiming at delivering high-accuracy light curves for many thousands of stars in search of planetary systems has also generated new insights in the field of variable stars and revived the interest of binary systems in general. The detection of eclipsing systems with pulsating components has particularly benefitted from this, and progress in this field is growing fast. In this review, we showcase some of the recent results obtained from studies of eclipsing systems with pulsating components based on data acquired by the space missions Kepler or TESS. We consider different system configurations including semi-detached eclipsing binaries in (near-)circular orbits, a (near-)circular and non-synchronized eclipsing binary with a chemically peculiar component, eclipsing binaries showing the heartbeat phenomenon, as well as detached, eccentric double-lined systems. All display one or more pulsating component(s). Among the great variety of known classes of pulsating stars, we discuss unevolved or slightly evolved pulsators of spectral type B, A or F and red giants with solar-like oscillations. Some systems exhibit additional phenomena such as tidal effects, angular momentum transfer, (occasional) mass transfer between the components and/or magnetic activity. How these phenomena and the orbital changes affect the different types of pulsations excited in one or more components, offers a new window of opportunity to better understand the physics of pulsations.

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“…These references include SB1, SB2 and wide binary systems. Up to now, no system harbouring an mCP stars is known with an orbital period less than 1.5 d. The number of known eclipsing binary systems hosting a magnetic CP star is still below five (Skarka et al, 2019). In summary, it can be said that up to 50% of all mCP stars are part of a binary system.…”

Section: Published Binary Fractionsmentioning

confidence: 97%

Binary fraction of magnetic chemically peculiar stars

Paunzen¹

2020

caosp

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Magnetic chemically peculiar stars of the upper main sequence are slowly rotating early B to early F-type objects with elemental overabundances of several orders of magnitude compared to the Sun. The driving mechanism is diffusion in the calm stellar atmosphere intensified by the presence of a stable organized magnetic field. The binary fraction is vital to understanding the formation and evolution of these objects as well as possible operating angular momentum loss mechanisms. The available literature on the binary fraction is reviewed and a list of needed future working steps is presented.

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HD 99458: First time ever Ap-type star as a δ Scuti pulsator in a short period eclipsing binary?

Cited by 22 publications

References 41 publications

A plethora of new, magnetic chemically peculiar stars from LAMOST DR4

A plethora of new, magnetic chemically peculiar stars from LAMOST DR4

Eclipsing Systems with Pulsating Components (Types β Cep, δ Sct, γ Dor or Red Giant) in the Era of High-Accuracy Space Data

Binary fraction of magnetic chemically peculiar stars

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