Blue Large-Amplitude Pulsators (BLAPs): Possible Origin, Evolutionary Status, and Nature of their Pulsations

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dc.contributor.editorCastanheira, B.
dc.contributor.editorVanderbosch, Z.
dc.contributor.editorMontgomery, M.
dc.creatorCorsico, A.H.
dc.creatorRomero, A.D.
dc.creatorAlthaus, L.G.
dc.creatorPelisoli, I.
dc.creatorKepler, S.O.
dc.date.accessioned2019-02-19T20:55:36Z
dc.date.available2019-02-19T20:55:36Z
dc.date.issued2018-07
dc.descriptionThe 21st European Workshop on White Dwarfs was held in Austin, TX from July 23rd to 27th of 2018en_US
dc.description.abstractThe Blue Large-Amplitude Pulsators (BLAPs) constitute a new class of pulsating stars. They are hot stars with effective temperatures of Teff ~ 30000 K and surface gravities of log g ~ 4.9, that pulsate with periods in the range 20 - 40 min. In Romero et al. (2018), we proposed that BLAPs are hot low-mass He-core pre-white dwarf (WD) stars that pulsate either in high-order non-radial g(gravity) modes or low-order radial modes, including the fundamental radial mode. The theoretical modes with periods in the observed range are unstable due to the k mechanism associated with the Z bump in the opacity at log T ~ 5.25. In this work, we extend the study of Romero et al. (2018) by assessing the rate of period changes of nonradial g modes and radial modes and comparing them with the values measured for BLAPs, in an attempt to validate the proposed evolutionary scenario, and to discern whether the observed modes are high-order g modes or radial modes.en_US
dc.description.departmentAstronomyen_US
dc.identifier.urihttps://hdl.handle.net/2152/73451
dc.identifier.urihttp://dx.doi.org/10.26153/tsw/603
dc.language.isoengen_US
dc.relation.ispartof21st European White Dwarf Workshopen_US
dc.rights.restrictionOpenen_US
dc.subjectwhite dwarfsen_US
dc.subjectBlue Large-Amplitude Pulsators (BLAPs)en_US
dc.titleBlue Large-Amplitude Pulsators (BLAPs): Possible Origin, Evolutionary Status, and Nature of their Pulsationsen_US
dc.typeConference paperen_US

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