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Spectral and photometric investigations of X-ray transient sources Barsukova, E.A., Burenkov, A.N., Borisov, N.V., Valeev, A.F., Klochkova, V.G., and Yushkin, M.V. (SAO RAN); Goranskij, V.P., and Metlova, N.V. (SAI, Moscow University)

- For scientific researches competition of SAO RAN

: Section: Astrophysical researches


Nature of X-ray transient sources
These are the objects that appear on the X-ray sky and then disappear what differs them from stationary sources.
These are the systems which contain compact components of different nature, white dwarf, neutron star or black hole. X-ray radiation appears due to accretion of matter on a compact object. Causes of X-ray outbursts: -Thermonuclear explosion of hydrogen on the surface of the white dwarf (CI Cam); -accumulation of matter in the accretion disk near a neutron star and falling of matter into magnetic poles of a neutron star where the thermonuclear burning initiates. Pulsar appears during X-ray outbursts, but it does not manifest itself in the quiet state (Be stars, BQ Cam, V490 Cep); -falling of low -mass bodies on a compact object due to gravitational capture (a comet nucleus or a meteoroid ) in the detached system (V934 Her, V4641 Sgr). Targets of this research are high-mass X-ray binaries, the purpose is to study the evolution of binary components and search of evolutionary traces in their spectra.

Be star and X-ray transient

Be star and circumstellar disk

Neutron star with an accretion disk on the orbit


1- , 60- 50- , 6- UAGS, NES SCORPIO. 3 5 .

2001 ­ 2012 .
.
Multicolor photometric observations of five HMXBs were performed in SAO RAS using 1 m Zeiss reflector, in SAI (Moscow University) Crimean Station 60 cm reflectors and 50 cm Maksutov telescope; and spectroscopic observations were carried out with the Russian 6 m BTA telescope with UAGS, NES, and SCORPIO spectrographs. Three of 5 presented objects were reserve targets in spectroscopic observing programs for BTA. The observations were performed in 2001 ­ 2012. We restore photometric history of five X-ray systems using photographic archives and applied digital reducing of images.


BQ Cam = V0332 +53 O8y-9oVe star + neutron star & pulsar on 34.2 da rbit O8-9Ve + , Ppuls = 4.375 s. P = 34.2 .
This X-ray outburst was predicted 9 months before (ATel 245)

9 ATel 245. - .

Accumulating disk in the system

-1000
Photometry began just after the date of the optical counterpart identification.

1983

1989

2004

2008 2010

.


BQ Cam:
Photometry and spectroscopy

X-ray outburst!

/SCORPIO. : -1000 ­ , ­ , ROTSE-III ( V) ­ , -600 ( ) ­ .


V490 Cep = Cep X-4 (GS 2138+56)
B1V-B2Ve + , Ppuls = 66.24 s 20.85 .
B1V-B2Ve star + neutron star & pulsar on the 20.85-day orbit

Cep X-4 (ROSAT/PSPC) 1993 . (Schulz et al., 1995)
X-ray images of Cep X-4 in quescence and outburst

V490 Cep (-1000)
V490 Cep in the optical range (Zeiss-1000)


Cep X-4:

Sonneberg

Research history on optical and X-rays


Moscow plate collection


SAO RAS & SAI MSU



1972

X-ray outbursts

1988

1993

1997

2002

2009


Discovery of optical variability


V490 Cep: UBVR
UBVR photometry & spectroscopy Optical outburst

X-ray outburst

Hg I Light pollution

/SCORPIO

- -1000 60-


V934 Her (HD 154791) = 4U 1700+24
M2 III + 415 . . .
M2 III type red giant + neutron star on the 415-day orbit, detaced system. No pulsar present.

V934 Her DSS, R, 5 5'
Optical image

UBV light curves & RXTE/ASM flux curve

1997

2002

UBV RXTE/ASM.


V934 Her:
Orbital light and X-ray flux variations 415-day phased light and flux curves

A
Amplitude spectra

Sp

RXTE/ASM

Mean flux curve


V934 Her:
Multi-periodic pulsations of the red giant

28.82
Pulsation with 28.82 day dominates

3 2009 ­ 2011 . Monitoring data of three seasons 2009-2011 ­ 4- . and model 4-component representation.


V934 Her:
-1000/
Zeiss-1000/UAGS spectrum and line profiles

2006.04.06

Gaudenzi & Polcaro (1999): .

profiles with wide emission and narrow absorption not confirmed because such a profiles are presented in a normal star.

-1000/ . 3 III SAO 63349.
This is a telluric band
2

UAGS line profiles


CI Cam = XTE J0421+560 B4 III-V[e] B4III-V[e] star + white dwarf
1998 .
Thermonuclear explosion on the white dwarf surface in 1998

HeII 4686A
Orbital elements of the white dwarf were determined using HeII 4686 emission

Kwd = 230 km/s = 51 km/s e = 0.62 p = 19.407 day T = JD 2452199.0 a·sin(i) = 48·106 km Fwd(M) = 12 M©

Radial velocity curve


CI Cam:
Historical light and X-ray flux curves

1962 - 1992

1998

1998 .
Orbital period before and after the 1998 outburst


CI Cam:
NEW 2012


Acceleration in the wind emission lines

[N II] 1998 . /. .
Profiles superimposed by their centers

[N II] line profile changes with time after the 1998 outburst (BTA/NES)

: ­ Fe II; [N II]; ­ Fe II; [N II]; [O I];


CI Cam: [e]-
Discovery of double-mode pulsations of B[e] star

Extracted light curves of pulsation modes

= 0.4152

= 0.2667

, .
Monitoring light curves




V4641 Sgr (SAX 1819.3-2525) B9A0 III c 6.5 + 9 = 2.817

B9-A0 III star + black hole of 9 solar mass on the 2.817 -day orbit Goranskij's star

GM Sgr

Luyten's star GM Sgr

VLA , R.Hjellming, 1999
VLA radio interferometry

1978
discovery

1999

2002 2003

2004

V4641 Sgr

Historical light curve of V4641 Sgr


V4641 Sgr: -
Archive photographic and multicolor CCD photometry

2007 . ( ). .
Appearance of reflection effect in may 2007 (red circles) SW IFT detected weak and variable Xray radiation.

Optical splashes detected

- .

- V R. .


V4641 Sgr:
Spectroscopy

- V4641 Sgr () , .

, -1000 . - .
Absorption H-alpha line is filled with emission.

/ . - .
The absorption component of a gas stream near the black hole was seen in H -alpha profile in the inferior conjunction


, .
Our research revealed big variety of properties and phenomena connected with presence of different-nature compact components in HMXBs.


Thanks for your attention