Statements (62)
| Predicate | Object |
|---|---|
| gptkbp:instance_of |
gptkb:star
|
| gptkbp:accretion |
can gain mass from companion stars
|
| gptkbp:advances |
advancements in research continue to reveal new insights.
|
| gptkbp:astrophysical_importance |
have significant astrophysical importance
|
| gptkbp:atmosphere |
may contain hydrogen or helium
|
| gptkbp:average_temperature |
10000 to 100000 K
|
| gptkbp:binary_systems |
can exist in binary systems
|
| gptkbp:color |
white to yellowish
|
| gptkbp:composed_by |
carbon and oxygen
|
| gptkbp:composed_of |
can show signs of planetary debris
|
| gptkbp:contains_star |
classified based on their spectra
|
| gptkbp:contribution_to_dark_matter |
may contribute to dark matter research
|
| gptkbp:cooling_system |
cooling rate varies with mass
|
| gptkbp:cosmological_implications |
have cosmological implications for the universe's fate
|
| gptkbp:discovery |
first identified in 1862
|
| gptkbp:distance |
up to several hundred light years
|
| gptkbp:end_state |
eventual cooling to black dwarf
|
| gptkbp:evolutionary_models |
studied in evolutionary models of stars
|
| gptkbp:evolutionary_track |
follow a specific evolutionary track in the Hertzsprung-Russell diagram
|
| gptkbp:example |
gptkb:Sirius_B
gptkb:Procyon_B 40 Eridani B |
| gptkbp:formed |
from the remnants of stars
|
| gptkbp:galactic_distribution |
found throughout the Milky Way
|
| gptkbp:has_luminosity |
low luminosity
influence stellar dynamics in their vicinity can interact with other stars in binary systems important in understanding stellar evolution |
| gptkbp:has_spectral_type |
DA, DB, DC, DQ, DZ
|
| https://www.w3.org/2000/01/rdf-schema#label |
White Dwarfs
|
| gptkbp:impact_on_supernovae |
can lead to Type Ia supernovae
|
| gptkbp:is_a_framework_for |
studied within theoretical frameworks of stellar evolution
|
| gptkbp:is_a_tool_for |
used as tools for studying the universe
|
| gptkbp:is_observed_in |
in various star clusters
|
| gptkbp:lifespan |
billions of years
|
| gptkbp:lighting |
faint
|
| gptkbp:magnetic_fields |
can have strong magnetic fields
|
| gptkbp:mass |
0.6 to 1.4 solar masses
part of the stellar population of galaxies |
| gptkbp:mass_limit |
gptkb:Chandrasekhar_limit
|
| gptkbp:mass-radius_relationship |
have a specific mass-radius relationship
|
| gptkbp:model |
studied in theoretical astrophysics
|
| gptkbp:nova |
can cause nova events when accreting material
|
| gptkbp:originated_in |
evolve from red giants
|
| gptkbp:planetary_nebulae |
often associated with planetary nebulae
|
| gptkbp:research |
gptkb:spectroscopy
difficult to observe due to faintness have a long observational history in astronomy observed using various observational techniques targeted in various observational campaigns |
| gptkbp:research_importance |
important for understanding the fate of stars
|
| gptkbp:role_in_cosmology |
used to measure distances
|
| gptkbp:rotation_period |
can rotate rapidly
|
| gptkbp:size |
similar to Earth
|
| gptkbp:spectral_analysis |
spectral analysis reveals their composition
|
| gptkbp:stellar_remnants |
one of the final stages of stellar evolution
|
| gptkbp:stellar_remnants_classification |
classified as stellar remnants in astrophysics
|
| gptkbp:support |
electron degeneracy pressure
|
| gptkbp:theoretical_predictions |
theoretical predictions match observations
|
| gptkbp:type |
gptkb:Supernova
|
| gptkbp:bfsParent |
gptkb:Supernova
|
| gptkbp:bfsLayer |
4
|