This HTML5 document contains 87 embedded RDF statements represented using HTML+Microdata notation.

The embedded RDF content will be recognized by any processor of HTML5 Microdata.

Namespace Prefixes

PrefixIRI
dctermshttp://purl.org/dc/terms/
dbohttp://dbpedia.org/ontology/
n11http://dbpedia.org/resource/File:
foafhttp://xmlns.com/foaf/0.1/
n14https://global.dbpedia.org/id/
schemahttp://schema.org/
dbthttp://dbpedia.org/resource/Template:
rdfshttp://www.w3.org/2000/01/rdf-schema#
n7http://commons.wikimedia.org/wiki/Special:FilePath/
rdfhttp://www.w3.org/1999/02/22-rdf-syntax-ns#
owlhttp://www.w3.org/2002/07/owl#
wikipedia-enhttp://en.wikipedia.org/wiki/
dbchttp://dbpedia.org/resource/Category:
dbphttp://dbpedia.org/property/
provhttp://www.w3.org/ns/prov#
xsdhhttp://www.w3.org/2001/XMLSchema#
wikidatahttp://www.wikidata.org/entity/
dbrhttp://dbpedia.org/resource/

Statements

Subject Item
dbr:AO_Serpentis
rdf:type
schema:Place dbo:Star dbo:Location dbo:Place owl:Thing dbo:CelestialBody
rdfs:label
AO Serpentis
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.
foaf:depiction
n7:AOSerLightCurve.png
dcterms:subject
dbc:Algol_variables dbc:A-type_main-sequence_stars dbc:Delta_Scuti_variables dbc:Eclipsing_binaries dbc:Durchmusterung_objects dbc:Serpens_(constellation) dbc:Objects_with_variable_star_designations
dbo:wikiPageID
66826049
dbo:wikiPageRevisionID
1080353788
dbo:wikiPageWikiLink
dbc:Objects_with_variable_star_designations dbc:A-type_main-sequence_stars dbr:Solar_cycle dbr:Richard_Prager dbr:Algol_variable dbc:Delta_Scuti_variables dbr:Stellar_parallax dbr:Orbital_period dbr:Photometric_system dbc:Eclipsing_binaries n11:AOSerLightCurve.png dbr:Apparent_visual_magnitude dbc:Durchmusterung_objects dbr:Light_curve dbr:All_Sky_Automated_Survey_for_SuperNovae dbr:Orbital_plane dbr:Semimajor_axis dbr:Roche_lobe dbr:Light_year dbr:Angular_momentum dbr:Binary_star dbc:Serpens_(constellation) dbr:Constellation dbr:Radius_of_the_Sun dbr:Paul_Guthnick dbr:Variable_star dbr:A-type_main-sequence_star dbr:Eclipsing_binary dbr:Cuno_Hoffmeister dbr:Serpens dbc:Algol_variables dbr:Delta_Scuti_variable
owl:sameAs
n14:Fr5ZR wikidata:Q88855783
dbp:wikiPageUsesTemplate
dbt:Odlist dbt:Convert dbt:Starbox_detail dbt:Starbox_end dbt:Starbox_character dbt:RA dbt:Starbox_orbit dbt:Starbox_image dbt:Starbox_observe dbt:Starbox_begin dbt:Starbox_catalog dbt:Starbox_astrometry dbt:DEC dbt:Starbox_reference dbt:Short_description dbt:Val dbt:Reflist dbt:Stars_of_Serpens
dbo:thumbnail
n7:AOSerLightCurve.png?width=300
dbp:bV
0.22
dbp:class
A2
dbp:component
Secondary Primary
dbp:constell
dbr:Serpens
dbp:epoch
J2000
dbp:pError
0.0229
dbp:parallax
2.2539
dbp:propMoDec
−10.444
dbp:propMoRa
−8.236
dbp:variable
dbr:Algol_variable dbr:Delta_Scuti_variable
dbo: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.
prov:wasDerivedFrom
wikipedia-en:AO_Serpentis?oldid=1080353788&ns=0
dbo:wikiPageLength
8998
foaf:isPrimaryTopicOf
wikipedia-en:AO_Serpentis