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Titolo:
An analysis of the light curve of the post common envelope binary MT Serpentis

Autore:

Indirizzi:: Lab Nacl Astrofis, BR-37500000 Itajuba, MG, Brazil Lab Nacl Astrofis Itajuba MG Brazil BR-37500000 BC000 Itajuba, MG, Brazil UFMG, ICEx, Dept Fis, BR-30123970 Belo Horizonte, MG, Brazil UFMG Belo Horizonte MG Brazil BR-30123970 BC70 Belo Horizonte, MG, Brazil USP, Inst Astron & Geofis, BR-01065970 Sao Paulo, Brazil USP Sao Paulo Brazil BR-01065970 BCGeofis, BR-01065970 Sao Paulo, Brazil
Titolo Testata:: ASTRONOMY & ASTROPHYSICS
fascicolo: 3, volume: 377, anno: 2001,
pagine: 898 - 910
SICI:: 1432-0746(200110)377:3<898:AAOTLC>2.0.ZU;2-7
Fonte:: ISI
Lingua:: ENG
Soggetto:: PLANETARY-NEBULAE; CENTRAL STAR; DISTANCES; SPECTROSCOPY; MAGNITUDES;
Keywords:: stars : variables : other stars : individual : MT Ser;
Tipo documento:: Article
Natura:: Periodico
Settore Disciplinare:: Physical, Chemical & Earth Sciences
Citazioni:: 23
Recensione:
Indirizzi per estratti:: Indirizzo: Bruch, A Lab Nacl Astrofis, CP 21, BR-37500000 Itajuba, MG, Brazil Lab Nacl Astrofis CP 21 Itajuba MG Brazil BR-37500000 BCG, Brazil



Citazione:: A. Bruch et al., "An analysis of the light curve of the post common envelope binary MT Serpentis", ASTRON ASTR, 377(3), 2001, pp. 898-910

Abstract

Photometric observations of MT Ser, the central star of the planetary nebula Abell 41 are presented. The periodic modulations detected by Grauer & Bond (1983) are confirmed, thus firmly establishing the binary nature of MT Ser. The significantly enlarged time base permits us to derive more accurateephemeris. The orbital period is either P-1 = 0.113226533 days or twice that value, P-2 = 0.226453066 days. We analyze the light curve (after a careful subtraction of the nebular contribution) with the Wilson-Devinney light curve synthesis routine. Since it is not a priori clear which is the true orbital period of MT Ser, two radically different models, one based on P-1 the other on P-2 are considered: (1) A low temperature component orbiting around a hot sub-dwarf. The variability is then due to a reflection effect together with ellipsoidal variations of one or both components. (2) Two hot sub-dwarfs of similar temperature and luminosity, partially eclipsing each other and exhibiting ellipsoidal variations. In both models, the primary as well as the secondary component are required to almost fill their respective Roche lobes. A contact configuration is possible. Pros and cons can be found for either of the two models. A final decision between them has to await the observations of a radial velocity curve. The orbital period is currently decreasing at a rate of (P) over dot/P = -1.15 x 10(-9) d(-1). Interpreting this as due to mass loss via a stellar winds permits us to estimate mass loss rates depending on the different model assumptions.

ASDD Area Sistemi Dipartimentali e Documentali, Università di Bologna, Catalogo delle riviste ed altri periodici
Documento generato il 25/05/13 alle ore 15:43:16