J/A+A/536/A27 AX Per UBVRI photometry (Skopal+, 2011)
Formation of a disk structure in the symbiotic binary AX Per during its
2007-10 precursor-type activity.
Skopal A., Tarasova T.N., Carikova Z., Castellani F., Cherini G.,
Dallaporta S., Frigo A., Marangoni C., Moretti S., Munari U., Righetti G.L.,
Siviero A., Tomaselli S., Vagnozzi A., Valisa P.
<Astron. Astrophys. 536, A27 (2011)>
=2011A&A...536A..27S 2011A&A...536A..27S
ADC_Keywords: Binaries, eclipsing ; Photometry, CCD ; Photometry, UBVRI
Keywords: stars: fundamental parameters - stars: winds, outflows -
stars: binaries: symbiotic - stars: individual: AX Per
Abstract:
AX Per is an eclipsing symbiotic binary. During active phases, deep
narrow minima are observed in its light curve, and the ionization
structure in the binary changes significantly. From ∼2007.5, AX Per
entered a new active phase. We aim to derive the ionization structure
in the binary and its changes during the recent active phase. We used
optical high- and low-resolution spectroscopy and UBVRcIc photometry.
We modeled the SED in the optical and broad wings of the H alpha line
profile during the 2007-10 higher level of the AX Per activity. After
10 orbital cycles (∼18.6 years), we again measured the eclipse of the
hot component by its giant companion in the light curve. We derived a
radius of 27±2R☉ for the eclipsed object and 115±2R☉
for the eclipsing cool giant. The new active phase was connected with
a significant enhancement of the hot star wind. From quiescence to
activity, the mass-loss rate increased from ∼9E-8 to ∼3E-6M☉/yr,
respectively. The wind causes the emission of the He++ zone, located
in the vicinity of the hot star, and also is the reason for the
fraction of the [OIII] zone at farther distances. Simultaneously, we
identified a variable optically thick warm (Teff∼6000K) source that
contributes markedly to the composite spectrum. The source was located
at the hot star's equator and has the form of a flared disk, whose
outer rim simulates the warm photosphere. The formation of the neutral
disk-like zone around the accretor during the active phase was
connected with its enhanced wind. It is probable that this connection
represents a common origin of the warm pseudophotospheres that are
indicated during the active phases of symbiotic stars.
Description:
The tables contain photometric B, V, Rc, Ic CCD observations as well
as photoelectric U, B, V observations of symbiotic binary AX Persei.
The dereddened emission line fluxes for several lines are also given.
Objects:
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RA (2000) DE Designation(s)
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01 36 22.7 +54 15 02 AX Per = V* AX Per
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 79 332 Photometric B, V, Rc, Ic CCD observations of
AX Persei
table3.dat 43 60 Photoelectric U, B, V observations of AX Persei
taken at the Skalnate Pleso Observatory
table5.dat 61 28 Dereddened emission line fluxes
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See also:
J/A+A/367/199 : UBVR photometry of AX Per (Skopal+, 2001)
J/MNRAS/399/2139 : CI Cyg BVRcIc light curves (Siviero+, 2009)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 3 I03 --- Tel Telescope identification in the ANS (1)
5- 15 F11.3 --- HJD Heliocentric Julian Date
17- 30 A14 "YYYY/MM/DD" Date Observation date
32- 37 F6.3 mag Vmag Johnson V magnitude
39- 43 F5.3 mag e_Vmag Error in Vmag
45- 49 F5.3 mag B-V ? Johnson B-V colour index
51- 55 F5.3 mag e_B-V ? Error in B-V
57- 61 F5.3 mag V-Rc ? Johnson-Cousins V-Rc colour index
63- 67 F5.3 mag e_V-Rc ? Error in V-Rc
69- 73 F5.3 mag V-Ic ? Johnson-Cousins V-Ic colour index
75- 79 F5.3 mag e_V-Ic ? Error in V-Ic
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Note (1): the Asiago Novae and Symbiotic Stars (ANS) Collaboration is an
italian network of amatorial and professional telescopes supervised by
the Asiago Observatory. The telescope codes are not explained.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 11 F11.3 --- HJD Heliocentric Julian Date
13- 22 A10 "YYYY/MM/DD" Date Observation date
24- 29 F6.3 mag Umag Magnitude U
31- 36 F6.3 mag Bmag ? Magnitude B
38- 43 F6.3 mag Vmag ? Magnitude V
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 11 F11.3 --- HJD Heliocentric Julian Date
13- 22 A10 "YYYY/MM/DD" Date Observation date
24- 26 F3.1 fW/m2 [OIII]1 ? Dereddened [OIII] (4363Å)
emission line flux
28- 31 F4.1 fW/m2 HeII Dereddened HeII (4686Å)
emission line flux
33- 36 F4.1 fW/m2 Hbeta Dereddened Hβ emission line flux
38- 40 F3.1 fW/m2 [OIII]2 ? Dereddened [OIII] (4950Å)
emission line flux
42- 44 F3.1 fW/m2 [OIII]3 ? Dereddened [OIII] (5007Å)
emission line flux
46- 49 F4.1 fW/m2 HeI ? Dereddened HeI (5875Å)
emission line flux
51- 53 F3.1 fW/m2 [FeVII] ? Dereddened [FeVII] (6087Å)
emission line flux
55- 59 F5.1 fW/m2 Halpha Dereddened Hα emission line flux
61 A1 --- Res [h/l] high- or low-resolution spectrum
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Acknowledgements:
Z. Caricova, zcarikova(at)ta3.sk
(End) Skopal, Carikova [AI SAS, Slovakia], Patricia Vannier [CDS] 14-Oct-2011