About: AO Serpentis

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http://dbpedia.org/describe/?url=http%3A%2F%2Fdbpedia.org%2Fresource%2FAO_Serpentis&graph=http%3A%2F%2Fdbpedia.org&graph=http%3A%2F%2Fdbpedia.org

AO Serpentis is an eclipsing binary star system in the Serpens Caput segment of the Serpens constellation. It is invisible to the naked eye with a typical apparent visual magnitude of 11.04. Variable star observers record a peak magnitude of 10.7, dropping to 12.0 during the primary eclipse and 10.8 from the secondary eclipse. The distance to this system is approximately 1,450 light years based on parallax measurements.

Attributes	Values
rdf:type	Thing place dbo:Location schema:Place celestial body star
rdfs:label	AO Serpentis (en)
rdfs:comment	AO Serpentis is an eclipsing binary star system in the Serpens Caput segment of the Serpens constellation. It is invisible to the naked eye with a typical apparent visual magnitude of 11.04. Variable star observers record a peak magnitude of 10.7, dropping to 12.0 during the primary eclipse and 10.8 from the secondary eclipse. The distance to this system is approximately 1,450 light years based on parallax measurements. (en)
foaf:depiction
dcterms:subject	A-type main-sequence stars Algol variables Delta Scuti variables Durchmusterung objects Eclipsing binaries Objects with variable star designations Serpens (constellation)
Wikipage page ID	66826049 (xsd:integer)
Wikipage revision ID	1080353788 (xsd:integer)
Link from a Wikipage to another Wikipage	Binary star Algol variable All Sky Automated Survey for SuperNovae Light curve A-type main-sequence stars Algol variables Delta Scuti variables Durchmusterung objects Eclipsing binaries Objects with variable star designations Serpens (constellation) Constellation Orbital plane Angular momentum Light year Delta Scuti variable Orbital period Stellar parallax A-type main-sequence star Cuno Hoffmeister Richard Prager Eclipsing binary Solar cycle Apparent visual magnitude Serpens Variable star Roche lobe Photometric system Paul Guthnick Semimajor axis Radius of the Sun
sameAs	AO Serpentis AO Serpentis
dbp:wikiPageUsesTemplate	dbt:Convert dbt:Reflist dbt:Short_description dbt:Starbox_astrometry dbt:Starbox_begin dbt:Starbox_catalog dbt:Starbox_character dbt:Starbox_detail dbt:Starbox_end dbt:Starbox_image dbt:Starbox_observe dbt:Starbox_orbit dbt:Starbox_reference dbt:Stars_of_Serpens dbt:Val dbt:DEC dbt:Odlist dbt:RA
thumbnail	wiki-commons:Special:FilePath/AOSerLightCurve.png?width=300
b-v	0.220000 (xsd:double)
class	A2 (en)
component	Primary (en) Secondary (en)
constell	Serpens
epoch	J2000 (en)
p error	0.022900 (xsd:double)
parallax	2.253900 (xsd:double)
prop mo dec	−10.444 (en)
prop mo ra	−8.236 (en)
variable	Algol variable Delta Scuti variable
has abstract	AO Serpentis is an eclipsing binary star system in the Serpens Caput segment of the Serpens constellation. It is invisible to the naked eye with a typical apparent visual magnitude of 11.04. Variable star observers record a peak magnitude of 10.7, dropping to 12.0 during the primary eclipse and 10.8 from the secondary eclipse. The distance to this system is approximately 1,450 light years based on parallax measurements. This system was discovered by C. Hoffmeister to be an Algol-type eclipsing binary in 1935. The following year, P. Guthnick and R. Prager reported a brightness variation between 10.5 and 12.0. In 2004, S. -L. Kim and associates determined that one of the components of this system is pulsating with a short period. This is a semi-detached binary star system with the secondary component completely filling its Roche lobe while the primary is 61% full. It has an orbital period of 21.1 hours and a semimajor axis of just 5.6 times the radius of the Sun. The orbital plane is inclined by an angle of 90° to the line of sight, causing the secondary component to be completely eclipsed once per orbit. The orbital period shows long-term cyclic variations, changing by up to 0.0051 days every 17.32 years. This may be due to magnetic activity cycles or the influence of a third body. The orbital period as a whole is steadily decreasing at the rate of (−5.39±0.03)×10−7 days yr−1 due to loss of mass and angular momentum by the system. The physical properties of the stellar components can be explained by a mass transfer. At some point in the past, mass flowed from the (at the time) more massive and evolved secondary component. This has left the primary as an A-type main-sequence star while the secondary is less massive but overly large. The hotter primary component is a Delta Scuti variable that is undergoing radial pulsation with a dominant frequency of 21.852 days−1 and a secondary frequency of 23.484 days−1. (en)
prov:wasDerivedFrom	wikipedia-en:AO_Serpentis?oldid=1080353788&ns=0
page length (characters) of wiki page	8998 (xsd:nonNegativeInteger)
foaf:isPrimaryTopicOf	wikipedia-en:AO_Serpentis
is Link from a Wikipage to another Wikipage of	List of stars in Serpens
is foaf:primaryTopic of	wikipedia-en:AO_Serpentis

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