The light and period changes of RT Andromedae
| dc.contributor.author | Erdem, A | |
| dc.contributor.author | Demircan, O | |
| dc.contributor.author | Güre, M | |
| dc.date.accessioned | 2025-01-27T20:27:02Z | |
| dc.date.available | 2025-01-27T20:27:02Z | |
| dc.date.issued | 2001 | |
| dc.department | Çanakkale Onsekiz Mart Üniversitesi | |
| dc.description.abstract | The nature of the long-term orbital period variation and the light level variation of RT And was studied based on all available photometric observations. The (O-C) diagram formed by all available times of eclipse minima could be either of a quasi-sinusoidal form superimposed on a parabolic form, or a long period sinusoidal form. The quasi-sinusoidal form with an amplitude of similar to0.002 days and a period of similar to 65 years could be due to a cyclic magnetic activity modulation on the orbital period of the system. Applegate's theory (Applegate 1992), in this case, predicts an similar to3 kG mean subsurface magnetic field for the primary component of the system. The parabolic form corresponds to a secular period decrease of about 3 x 10(-9) m(circle dot) yr(-1) caused by mass loss from the system, and the long-period sinusoidal form with an amplitude of similar to0.02 days and a period of similar to 105 years corresponds to a secular period change caused by the light-time effect due to an unseen third star in the system. It was estimated that the unseen third star should be a low mass (lower than 0.6 m(circle dot)) and faint (similar to5.(m) fainter than the system RT And) star, whose detection is almost impossible. Future data will add information on the nature of the secular (O-C) variation. Secular light level variation of the system was found to be irregular and no correlation was detected with the orbital period variation. | |
| dc.identifier.doi | 10.1051/0004-6361:20011357 | |
| dc.identifier.endpage | 883 | |
| dc.identifier.issn | 0004-6361 | |
| dc.identifier.issue | 3 | |
| dc.identifier.scopus | 2-s2.0-0035625728 | |
| dc.identifier.scopusquality | Q1 | |
| dc.identifier.startpage | 878 | |
| dc.identifier.uri | https://doi.org/10.1051/0004-6361:20011357 | |
| dc.identifier.uri | https://hdl.handle.net/20.500.12428/22556 | |
| dc.identifier.volume | 379 | |
| dc.identifier.wos | WOS:000172505100014 | |
| dc.identifier.wosquality | Q2 | |
| dc.indekslendigikaynak | Web of Science | |
| dc.indekslendigikaynak | Scopus | |
| dc.language.iso | en | |
| dc.publisher | Edp Sciences S A | |
| dc.relation.ispartof | Astronomy & Astrophysics | |
| dc.relation.publicationcategory | info:eu-repo/semantics/openAccess | |
| dc.rights | info:eu-repo/semantics/openAccess | |
| dc.snmz | KA_WoS_20250125 | |
| dc.subject | stars : binaries : eclipsing | |
| dc.subject | stars : individual : RT And | |
| dc.title | The light and period changes of RT Andromedae | |
| dc.type | Article |
