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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
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: -------------------------------------------- RA (2000) DE Designation(s) -------------------------------------------- 01 36 22.7 +54 15 02 AX Per = V* AX Per -------------------------------------------- File Summary:
FileName Lrecl Records Explanations
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
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
Bytes Format Units Label Explanations
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
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.
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
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
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
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
Acknowledgements: Z. Caricova, zcarikova(at)ta3.sk
(End) Skopal, Carikova [AI SAS, Slovakia], Patricia Vannier [CDS] 14-Oct-2011
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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