Optical and X-ray Behavior of the High Mass X-ray Transient A0535+26/HDE245770 in 2014

• Autorzy: Giovannelli F. , Bisnovatyi-Kogan G. S. , Bruni I. , Corfini G. , Martinelli F. , Rossi C.
• Języki publikacji: EN

Abstrakty

EN

The optical behavior of the Be star in the high-mass X-ray transient A0535+26/HDE245770 shows that at periastron the luminosity is typically enhanced by 0.02 mag to a few tenths mag, and the X-ray outburst occurs eight days after the periastron. Indeed, at the periastron an increase of the mass flux occurs. This sort of flush reaches the external part of the temporary accretion disk around the neutron star and moves to the hot central parts of the accretion disk and the neutron star's surface. The time necessary for this process is dependent on the turbulent viscosity in the accretion disk. In this paper we will show the behavior of this system in optical band around the predicted periastron passages in 2014, by using the ephemeris - JD_opt-outb = JD₀(2 444 944)±n(111.0±0.4) days - that we used to schedule our spectroscopic and photometric optical observations. Spectroscopic unusual activity detected in the Balmer lines and the enhancement in the emission in B, V, and R bands around the 106th periastron passage, and in V-band around the 108th periastron passage after the "zero event" 811205-E at JD 2 444 944, and the subsequent X-ray events definitively demonstrate the existence of a ≈8-day delay between optical and X-ray flares.

Słowa kluczowe

EN

X-rays: binaries; accretion, accretion disks; stars: neutron; stars: emission line; stars:Be; stars: individual: A0535+26

• Wydawca: Copernicus Foundation for Polish Astronomy
• Czasopismo: Acta Astronomica
• Rocznik: 2015
• Tom: Vol. 65, No. 1
• Strony: 107--116
• Opis fizyczny: Bibliogr. 41 poz., wykr.

Twórcy

autor

Giovannelli F.

• INAF - Istituto di Astrofisica e Planetologia Spaziali, Area di Ricerca di Roma-2, Viadel Fosso del Cavaliere 100, I 00133 Roma, Italy

autor

Bisnovatyi-Kogan G. S.

• Space Research Institute, Profsoyuznaya 84/32, Moscow 117810, Russia
• National Research Nuclear University MEPhI, Kashirskoe Shosse 31, Moscow 115409, Russia

autor

Bruni I.

• INAF - Osservatorio Astronomico di Bologna, Stazione astronomica di Loiano, Stradadella Futa (SS N. 65) - I 40050 Loiano, Italy

autor

Corfini G.

• Montecatini Val di Cecina Astronomical Centre - Loc. Palareta, 18 I 56040 Montecatini Val di Cecina, Italy

autor

Martinelli F.

• Montecatini Val di Cecina Astronomical Centre - Loc. Palareta, 18 I 56040 Montecatini Val di Cecina, Italy

autor

Rossi C.

• Dept. of Physics, Roma Sapienza University, - P.le Aldo Moro 2 - I 00185 Roma, Italy

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