Statements (55)
| Predicate | Object |
|---|---|
| gptkbp:instance_of |
gptkb:star
|
| gptkbp:bfsLayer |
4
|
| gptkbp:bfsParent |
gptkb:White_Dwarf
gptkb:Chandrasekhar_limit |
| gptkbp:area |
about 0.01 solar radii
|
| gptkbp:atmosphere |
can contain hydrogen or helium
|
| gptkbp:average_temperature |
up to 100,000 K
|
| gptkbp:characteristics |
often appear as point sources in the sky
|
| gptkbp:color |
white to yellowish
|
| gptkbp:composed_of |
carbon and oxygen
can vary widely among different stars |
| gptkbp:constellation |
final stage of low to intermediate mass stars
|
| gptkbp:contains |
part of the Hertzsprung-Russell diagram
|
| gptkbp:cooling_system |
depends on mass and composition
|
| gptkbp:discovered_by |
first identified in 1850s
|
| gptkbp:distance |
can be several light-years away
|
| gptkbp:distribution |
found in various regions of the galaxy
|
| gptkbp:ecological_role |
contribute to the chemical enrichment of the galaxy
|
| gptkbp:end_of_life |
eventually become black dwarfs
|
| gptkbp:environment |
planetary nebulae
|
| gptkbp:example |
gptkb:Sirius_B
|
| gptkbp:formed |
post-main sequence evolution
|
| gptkbp:has_impact_on |
important for understanding the fate of stars.
|
| gptkbp:has_luminosity |
decreases over time
|
| gptkbp:has_spectral_type |
DA, DB, DC, etc.
used to determine atmospheric composition |
| gptkbp:historical_significance |
first evidence of stellar evolution
|
| https://www.w3.org/2000/01/rdf-schema#label |
white dwarf stars
|
| gptkbp:is_a_fusion_of |
no longer undergo fusion reactions
|
| gptkbp:is_compared_to |
more massive than neutron stars but less than black holes
|
| gptkbp:lifespan |
billions of years
|
| gptkbp:lighting |
faint
|
| gptkbp:location |
found in binary systems
|
| gptkbp:losses |
occurs during the red giant phase
|
| gptkbp:mass |
gptkb:Chandrasekhar_limit
0.17 to 1.33 solar masses part of the Milky Way's stellar population up to 1.4 solar masses |
| gptkbp:notable_event |
gptkb:Procyon_B
|
| gptkbp:notable_feature |
high density
|
| gptkbp:number_of_cores |
mostly crystalline carbon and oxygen
|
| gptkbp:operating_system |
can accrete material from companion stars
|
| gptkbp:origin |
formed from stars that have exhausted their nuclear fuel
|
| gptkbp:related_concept |
gptkb:Type_Ia_supernovae
|
| gptkbp:related_model |
used to predict their evolution
|
| gptkbp:research |
photometry and spectroscopy
ongoing research in astrophysics Hubble Space Telescope, Gaia faintness makes them hard to detect |
| gptkbp:research_focus |
important for understanding stellar evolution
|
| gptkbp:state |
cooling and fading over time
|
| gptkbp:supports |
electron degeneracy pressure
|
| gptkbp:theory |
models predict cooling timescales
|
| gptkbp:track |
follows a specific path on the HR diagram
|
| gptkbp:type |
gptkb:nebula
|