About: BH Crucis

Facets (new session)
Description
Metadata
Settings
- Rule:
- Inverse Functional Properties:
- "Same As":

About: BH Crucis Goto Sponge NotDistinct Permalink

An Entity of Type : dbo:Star, within Data Space : dbpedia.demo.openlinksw.com associated with source document(s)
QRcode icon

http://dbpedia.demo.openlinksw.com/c/5HXD4Dmmgk

BH Crucis, also known as Welch's Red Variable, is a star in the constellation Crux. A long period (Mira-type) variable, its apparent magnitude ranges from 6.6 to 9.8 over 530 days. Hence at its brightest it is barely visible with the unaided eye in a rural sky. A red giant, it had been classified ranging between spectral types SC4.5/8-e and SC7/8-e, but appears to have evolved into a C-type (carbon star) spectrum by 2011.

Attributes	Values
rdf:type	Thing place dbo:Location schema:Place celestial body star
rdfs:label	BH Crucis (en)
rdfs:comment	BH Crucis, also known as Welch's Red Variable, is a star in the constellation Crux. A long period (Mira-type) variable, its apparent magnitude ranges from 6.6 to 9.8 over 530 days. Hence at its brightest it is barely visible with the unaided eye in a rural sky. A red giant, it had been classified ranging between spectral types SC4.5/8-e and SC7/8-e, but appears to have evolved into a C-type (carbon star) spectrum by 2011. (en)
foaf:name	BH Crucis (en)
foaf:depiction
dct:subject	Astronomical objects discovered in 1969 Emission-line stars Hipparcos objects Objects with variable star designations Stars with proper names S-type stars Crux (constellation) Carbon stars Mira variables
Wikipage page ID	43122887 (xsd:integer)
Wikipage revision ID	1084602866 (xsd:integer)
Link from a Wikipage to another Wikipage	Carbon Mira variable Light curve Astronomical objects discovered in 1969 Emission-line stars Hipparcos objects Objects with variable star designations Stars with proper names Constellation Crux Apparent magnitude Star Photographic plate S-type stars Absolute magnitude Carbon star Red giant Asymptotic giant branch Technetium Crux (constellation) Carbon stars Mira variables Sonneberg Observatory Photometric system RV Tauri variable Gaia Data Release 2
sameAs	BH Crucis BH Crucis BH Crucis BH Crucis
dbp:wikiPageUsesTemplate	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_reference dbt:Val dbt:DEC dbt:Odlist dbt:RA dbt:Stars_of_Crux
thumbnail	wiki-commons:Special:FilePath/BHCruLightCurve.png?width=300
appmag v	6.550000 (xsd:double)
class	(en) SC4.5/8-e - SC7/8-e (en)
constell	Crux
epoch	J2000.0 (en)
gravity	−0.02 (en)
luminosity	13700 (xsd:integer)
mass	2.550000 (xsd:double)
metal fe	−0.14 (en)
p error	0.052900 (xsd:double)
parallax	0.995200 (xsd:double)
radius	216 (xsd:integer)
temperature	3000 (xsd:integer)
type	Asymptotic giant branch
variable	Mira variable
has abstract	BH Crucis, also known as Welch's Red Variable, is a star in the constellation Crux. A long period (Mira-type) variable, its apparent magnitude ranges from 6.6 to 9.8 over 530 days. Hence at its brightest it is barely visible with the unaided eye in a rural sky. A red giant, it had been classified ranging between spectral types SC4.5/8-e and SC7/8-e, but appears to have evolved into a C-type (carbon star) spectrum by 2011. Ronald G. Welch discovered the star while looking for new variables in October 1969. In the first thirty years since discovery, it has become redder and brighter (mean magnitude changing from 8.047 to 7.762) and its period lengthened by 25% from 421 to 530 days. Retrospective examination of photographic plates taken in South West Africa in 1937 and 1951 and stored at Sonneberg Observatory suggest the amplitude of variation might have been smaller in the earliest records. A study of the star published in 2011 found that the increase in period appeared to have stopped or even begun reversing (estimated at 524 days in 2011), and that the spectral class had changed from SC to C, with carbon emission becoming more prominent. Technetium was also recorded in the emission spectrum and its surface temperature deemed to have cooled to 3000 K. Unusually for a Mira variable, BH Crucis had a double maximum, with two peaks in brightness, reminiscent of an RV Tauri variable. However, with the lengthening of its period, this feature disappeared. Guandalini and Cristallo calculated the luminosity of Mira variables based on their periods. Using a period of 421 days, they calculated the absolute magnitude of BH Crucis to be -4.80. Uttenthaler and colleagues calculated a bolometric magnitude of -5.59. Gaia Data Release 2 gives a parallax of 0.9952 mas and a corresponding distance of around 1000 pc. (en)
gold:hypernym	Star
prov:wasDerivedFrom	wikipedia-en:BH_Crucis?oldid=1084602866&ns=0
page length (characters) of wiki page	7695 (xsd:nonNegativeInteger)
foaf:isPrimaryTopicOf	wikipedia-en:BH_Crucis
is Link from a Wikipage to another Wikipage of	Crux S-type star List of stars in Crux
is foaf:primaryTopic of	wikipedia-en:BH_Crucis

Faceted Search & Find service v1.17_git147 as of Sep 06 2024

Alternative Linked Data Documents: ODE Content Formats:

RDF

ODATA

Microdata

About

OpenLink Virtuoso version 08.03.3331 as of Sep 2 2024, on Linux (x86_64-generic-linux-glibc212), Single-Server Edition (378 GB total memory, 53 GB memory in use)
Data on this page belongs to its respective rights holders.
Virtuoso Faceted Browser Copyright © 2009-2024 OpenLink Software