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BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20180726T103000
DTEND;TZID=Atlantic/Canary:20180726T113000
UID:iactalks-1184
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/1184
CREATED:2018-07-26T10:30:00+01:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY:Distribution of the Wind from the Cool Giants in Symbiotic Binary S
 tars
DESCRIPTION:Distribution of the Wind from the Cool Giants in Symbiotic Bina
 ry Stars\nDr. Natalia Shagatova\n\nIn symbiotic stars, two different physi
 cal regimes of circumstellarmaterial exist side by side. Around the donor 
 red giant star, there is acool and dense conical region of neutral wind. D
 uring quiescent phases,the rest of the wind from the donor is ionized by i
 ts companion, in mostcases, a very hot and luminous white dwarf powered by
  accretion from thegiant's wind. Mass outflow from the majority of cool co
 mponents insymbiotic binaries is still not understood well. Some informati
 on aboutthe distribution of circumstellar matter can be obtained by measur
 ing theneutral hydrogen column densities from Rayleigh scattering along th
 emultiple lines of sight. I will present the wind velocity profiles derive
 dfrom the measured column densities of neutral hydrogen for two quiethigh-
 inclination symbiotic systems, EG And and SY Mus. The column densitymodels
  indicate the wind focusing towards the orbital plane and allow toinvestig
 ate the origin of the asymmetric UV continuum light curve profilesof symbi
 otic stars.
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