On the existence of 'Maia variables'
| dc.authorid | Ozuyar, Dogus/0000-0001-8544-0950 | |
| dc.contributor.author | Alicavus, Filiz Kahraman | |
| dc.contributor.author | Handler, Gerald | |
| dc.contributor.author | Chowdhury, Sowgata | |
| dc.contributor.author | Niemczura, Ewa | |
| dc.contributor.author | Jayaraman, Rahul | |
| dc.contributor.author | De Cat, Peter | |
| dc.contributor.author | Ozuyar, Dogus | |
| dc.date.accessioned | 2025-01-27T20:53:55Z | |
| dc.date.available | 2025-01-27T20:53:55Z | |
| dc.date.issued | 2024 | |
| dc.department | Çanakkale Onsekiz Mart Üniversitesi | |
| dc.description.abstract | There are different classes of pulsating stars in the H-R diagram. While many of those classes are undisputed, some remain a mystery such as the objects historically called 'Maia variables'. Whereas the presence of such a class was suggested seven decades ago, no pulsational driving mechanism is known that could excite short-period oscillations in these late B to early A-type stars. Alternative hypotheses that would render the reports of variability of those stars erroneous have been proposed such as incorrect effective temperatures, binarity or rapid rotation, but no certain conclusions have been reached yet. Therefore, the existence of these variables as a homogeneous class of pulsating star is still under discussion. Meanwhile, many new candidates of these variables have been claimed especially by using photometric observations of space telescopes. In this study, we examined 31 objects that are alleged members of this hypothetical group and carried out detailed spectroscopic and photometric analyses to test the proposed hypotheses for their cause of variability. The T-eff, log g , v sin i , and chemical abundances of the targets were determined and the TESS photometric data were examined. As a result, we found that most of these targets are located inside the delta Scuti, beta Cephei, or SPB star instability strips, a few show evidence for binarity and others for rapid rotation. We give arguments that none of the apparently rapid pulsations in our targets is caused by a star outside any known instability strip. By extrapolation, we argue that most stars proposed as pulsators outside well-established instability domains are misclassified. Hence there is no sufficient evidence justifying the existence of a class of pulsating stars formerly known as the 'Maia variables'. | |
| dc.description.sponsorship | Scientific and Technological Research Council (TUBITAK) [121F474]; Polish National Center for Science (NCN) [2015/18/A/ST9/00578, 2021/43/B/ST9/02972]; Horizon 2020: (OPTICON); European Union [730890, 214]; NASA Explorer Program | |
| dc.description.sponsorship | The authors would like to thank the reviewer for useful comments and suggestions that helped to improve the publication. This study has been supported by the Scientific and Technological Research Council (TUBITAK) project 121F474. GH thanks the Polish National Center for Science (NCN) for supporting the study through grants 2015/18/A/ST9/00578 and 2021/43/B/ST9/02972. Horizon 2020: (OPTICON) This project has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 730890. The calculations have been partly carried out using resources provided by the Wroc & lstrok;aw Centre for Networking and Supercomputing (http://www.wcss.pl), Grant No 214. This material reflects only the authors views and the Commission is not liable for any use that may be made of the information contained therein. Based on observations made with the Mercator Telescope, operated on the island of La Palma by the Flemish Community, at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofsica de Canarias. The TESS data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). Funding for the TESS mission is provided by the NASA Explorer Program. This work has made use of data from the European Space Agency (ESA) mission Gaia (http://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, http://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular, the institutions participating in the Gaia Multilateral Agreement. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. We are grateful to Vichi Antoci, Tim Bedding, Dominic Bowman, Don Kurtz, Nami Mowlavi and Simon Murphy for their comments on a draft version of this paper. | |
| dc.identifier.doi | 10.1017/pasa.2024.76 | |
| dc.identifier.issn | 1323-3580 | |
| dc.identifier.issn | 1448-6083 | |
| dc.identifier.scopus | 2-s2.0-85209735586 | |
| dc.identifier.scopusquality | Q1 | |
| dc.identifier.uri | https://doi.org/10.1017/pasa.2024.76 | |
| dc.identifier.uri | https://hdl.handle.net/20.500.12428/25904 | |
| dc.identifier.volume | 41 | |
| dc.identifier.wos | WOS:001347991000001 | |
| dc.identifier.wosquality | N/A | |
| dc.indekslendigikaynak | Web of Science | |
| dc.indekslendigikaynak | Scopus | |
| dc.language.iso | en | |
| dc.publisher | Cambridge Univ Press | |
| dc.relation.ispartof | Publications of The Astronomical Society of Australia | |
| dc.relation.publicationcategory | info:eu-repo/semantics/openAccess | |
| dc.rights | info:eu-repo/semantics/openAccess | |
| dc.snmz | KA_WoS_20250125 | |
| dc.subject | Stars: oscillations | |
| dc.subject | stars: variables: general | |
| dc.subject | techniques: photometric | |
| dc.subject | techniques: spectroscopic | |
| dc.title | On the existence of 'Maia variables' | |
| dc.type | Article |
