Searches , social queries for PRE STELLAR-CORE
Search references for PRE STELLAR-CORE. Phrases containing PRE STELLAR-CORE
See searches and references containing PRE STELLAR-CORE!
Search references for PRE STELLAR-CORE. Phrases containing PRE STELLAR-CORE
See searches and references containing PRE STELLAR-CORE!PRE STELLAR-CORE
Phase in the formation of low-mass stars
Pre-stellar cores are the nurseries of new stars, and are an early phase in the formation of low-mass stars, before gravitational collapse produces a
Pre-stellar_core
Region at the center of a star
A stellar core is the extremely hot, dense region at the center of a star. For an ordinary main sequence star, the core region is the volume where the
Stellar_core
Pre-stellar core in the constellation Serpens
L183 or L134N is a pre-stellar core in the constellation Serpens Cauda 360 light-years away. This massive accumulation of gas and dust was the interstellar
L183
Large self-illuminated object in space
ceases and its core becomes a stellar remnant: a white dwarf, a neutron star, or—if it is sufficiently massive—a black hole. Stellar nucleosynthesis
Star
Binary systems of planetary-mass objects
JuMBOs may form when radiation from massive stars erodes fragmenting pre-stellar cores through a process called photoerosion. In this scenario, Lyman continuum
Jupiter-mass_binary_object
Changes to stars over their lifespans
Stellar evolution is the process by which a star changes over the course of time. Depending on the mass of the star, its lifetime can range from a few
Stellar_evolution
Early stage in the process of star formation
largest pre-main-sequence stars are also of modest size. Star formation begins in relatively small molecular clouds called dense cores. Each dense core is
Protostar
Creation of chemical elements within stars
In astrophysics, stellar nucleosynthesis is the creation of chemical elements by nuclear reactions within stars. Stellar nucleosynthesis has occurred
Stellar_nucleosynthesis
Chemical compound
Spezzano, S.; Leonardo, E. (2014-09-01). "Deuterated methanol in the pre-stellar core L1544". Astronomy & Astrophysics. 569: A27. arXiv:1408.2491. Bibcode:2014A&A
Deuterated_methanol
infrared light scattered by unusually large grains of dust in the denser core regions of molecular clouds and which evidently begin their growth before
Coreshine
Outer region of the volume of a star
The stellar atmosphere is the outer region of the volume of a star, lying above the stellar core, radiation zone and convection zone. The stellar atmosphere
Stellar_atmosphere
Central region of the Sun
through a better understanding of neutrino oscillation. Active region Stellar core García, Rafael A.; Turck-Chièze, Sylvaine; Jiménez-Reyes, Sebastian J
Solar_core
Fictional character in Stellar Blade
is a character introduced in and the protagonist of the 2024 video game Stellar Blade by developer Shift Up, and created by Kim Hyung Tae. Eve is a soldier
Eve_(Stellar_Blade)
Hypothetical early-universe star with a black hole core
such an object would have resulted from the core of a large supermassive protostar collapsing into a stellar-mass black hole, where the outer layers of
Quasi-star
Flow of gas ejected from the upper atmosphere of a star
A stellar wind is a flow of gas ejected from the upper atmosphere of a star. It is distinguished from the bipolar outflows characteristic of young stars
Stellar_wind
Chemical compound
outer edge of the core to the center. This showed that even N2H+ is not an ideal tracer for the chemistry of dense pre-stellar cores, and concluded that
Diazenylium
Grouping of stars by similar metallicity
1944, Walter Baade categorized groups of stars within the Milky Way into stellar populations. In the abstract of the article by Baade, he recognizes that
Stellar_population
Sky region containing dark interstellar clouds
containing numerous protostars. Due to the large number of protostars and pre-stellar cores in the region, it is likely that Serpens South has the most star-formation
Serpens–Aquila_Rift
Star in the stage when it has not yet reached the main sequence
blows away this envelope, it is optically visible, and appears on the stellar birthline in the Hertzsprung-Russell diagram. At this point, the star has
Pre-main-sequence_star
Path taken by pre-main-sequence stars in the Hertzsprung–Russell diagram
radiative core, as the core does not become hot enough, and instead, will remain on the Hayashi track until it reaches the main sequence. Stellar evolution
Henyey_track
Astrophysical phenomenon
companion through accretion, or by a stellar merger. In the case of a massive star's sudden implosion, the core of a massive star will undergo sudden
Supernova
Region of a star
radiative zone. From 0.3 to 1.2 solar masses, the region around the stellar core is a radiative zone, separated from the overlying convection zone by
Radiative_zone
Continuous band of stars that appears on plots of stellar color versus brightness
stellar color versus brightness as a continuous and distinctive band. Stars spend the majority of their lives on the main sequence, during which core
Main_sequence
Stellar classification
and white dwarfs which are much more common, the last of which being stellar remnants). A G-type main-sequence star with the mass of the Sun will fuse
G-type_main-sequence_star
Scatter plot of stars showing the relationship of luminosity to stellar classification
relationship between the stars' absolute magnitudes or luminosities and their stellar classifications or effective temperatures. It is also sometimes called
Hertzsprung–Russell_diagram
Classification of stars based on spectral properties
In astronomy, stellar classification is the classification of stars based on their spectral characteristics. Electromagnetic radiation from the star is
Stellar_classification
Structure of stars
Stellar structure models describe the internal structure of a star in detail and make predictions about the luminosity, the color and the future evolution
Stellar_structure
Black hole formed by a collapsed star
A stellar black hole (or stellar-mass black hole) is a black hole formed by the gravitational collapse of a star. They have masses ranging from about five
Stellar_black_hole
Mass of a star in astronomy
ending in a core-collapse supernova explosion.[dubious – discuss] Black holes created as a result of a stellar collapse are termed stellar-mass black holes
Stellar_mass
Study of the movement of stars
In astronomy, stellar kinematics is the observational study or measurement of the kinematics or motions of stars through space. Stellar kinematics encompasses
Stellar_kinematics
Stellar core remnant
white dwarf star accumulates sufficient material from a stellar companion to raise its core temperature enough to ignite carbon fusion, it will undergo
White_dwarf
Gravitational process studied in astronomy
within molecular clouds in interstellar space—sometimes referred to as "stellar nurseries" or "star-forming regions"—collapse and form stars. As a branch
Star_formation
Brief thermal runaway nuclear fusion in the core of low-mass stars
of stellar evolution in stars with less than 2.0 M☉, the nuclear fusion of hydrogen ceases in the core as it is depleted, leaving a helium-rich core. Hydrogen
Helium_flash
Classification in astronomy
"compact-object mergers and magnetars arising from normal core collapse supernovae". The usual endpoint of stellar evolution is the formation of a compact star. Every
Compact_object
Magnetic field generated inside a star
10Be in ice cores—have established substantial magnetic variability of the Sun on decadal, centennial and millennial time scales. Stellar magnetic fields
Stellar_magnetic_field
Star in its early stage of evolution
Young stellar object (YSO) denotes a star in its early stage of evolution. This class consists of two groups of objects: protostars and pre-main-sequence
Young_stellar_object
Dark nebula in constellation Perseus
outflow. Towards the east is the source IRS 2E, a source between a pre-stellar core and a protostar. The source IRS 3B was studied the most and ALMA showed
Barnard_203
Orbital satellite telescope
clouds. The first detection of the earliest stages of stellar formation. The pre-stellar core L1689B was found and studied in great detail with ISO's
Infrared_Space_Observatory
Grouping of evolved cool luminous stars
to circulate core material to the surface. AGB stars are typically long-period variables, and suffer mass loss in the form of a stellar wind. For M-type
Asymptotic_giant_branch
Changed position of star vs background
Stellar parallax is the apparent shift of position (parallax) of any nearby star (or other object) against the background of distant stars. By extension
Stellar_parallax
Portion of the giant branch before helium ignition
stellar evolution. It is a stage that follows the main sequence for low- to intermediate-mass stars. Red-giant-branch stars have an inert helium core
Red-giant_branch
Supernova that ejects a large mass at unusually high velocity
being studied as the best method for both stripping stellar envelopes to leave a bare carbon-oxygen core, and for inducing the necessary spin conditions to
Hypernova
Hypothetical class of star that develops from a red dwarf
stars. Simulations have been conducted on the evolution of red dwarfs with stellar mass between 0.06 M☉ and 0.25 M☉. Of the masses simulated, the bluest of
Blue_dwarf_(red-dwarf_stage)
Stellar classification
Thomas (2013). "The stellar and sub-stellar initial mass function of simple and composite populations". Planets, Stars, and Stellar Systems. pp. 115–242
O-type_star
2026 studio album by XG
Neil Z., THE CORE - 核 - XG | Album | AllMusic, AllMusic, retrieved March 28, 2026 "XG is Back With Stellar Full-Length Album THE CORE - 核". The Kraze
The_Core_(XG_album)
Methods for estimating the age of a star
in stellar age estimation, an attempt to identify within reasonable degrees of confidence what the age of a star is. These methods include stellar evolutionary
Stellar_age_estimation
Physical phenomenon of stars
Stellar mass loss is a phenomenon observed in stars by which stars lose some mass over their lives. Mass loss can be caused by triggering events that
Stellar_mass_loss
Stage of stellar evolution
The horizontal branch (HB) is a stage of stellar evolution that immediately follows the red-giant branch in stars whose masses are similar to the Sun's
Horizontal_branch
Type of star larger than main-sequence but smaller than a giant
Maurizio; Cassisi, Santi (2005). "Evolution of Stars and Stellar Populations". Evolution of Stars and Stellar Populations: 400. Bibcode:2005essp.book.....S. Pols
Subgiant
Stellar classification distinguished by bright blue luminosity
Acrux. This class of stars was introduced with the Harvard sequence of stellar spectra and published in the Revised Harvard photometry catalogue. The
B-type_main-sequence_star
Type of large cool star
intermediate mass (roughly 0.3–8 solar masses (M☉)) in a late phase of stellar evolution. The outer atmosphere is inflated and tenuous, making the radius
Red_giant
Type of emission nebula created by dying red giants
of stellar evolution. Once all of the red giant's atmosphere has been dissipated, energetic ultraviolet radiation from the exposed hot luminous core, called
Planetary_nebula
Outermost layer of a star's atmosphere
Scientists have greater access to the solar corona than they do to other stellar coronae, since it is inside our solar system. This means that the coronae
Stellar_corona
Cavity of hot gas blown from a star
A stellar-wind bubble is a cavity light-years across filled with hot gas blown into the interstellar medium by the high-velocity (several thousand km/s)
Stellar-wind_bubble
Stars that appear green
high signal-to-noise ratio. Its modelled colour also varies across the stellar disc, with subtle differences in hue toward the outer limb. Its green appearance
Green_star_(astronomy)
ultraviolet–optical flare from the tidal disruption of a helium-rich stellar core". Nature. 485 (7397): 217–220. arXiv:1205.0252. Bibcode:2012Natur.485
Timeline_of_stellar_astronomy
Stage in the evolution of some stars
into the outer layers of the star's atmosphere, where they can be seen in stellar spectra. The first dredge-up The first dredge-up occurs when a main-sequence
Dredge-up
Main sequence star that is more luminous and bluer than expected
that is more luminous and bluer than expected. Typically identified in a stellar cluster, they have a higher effective temperature than the main sequence
Blue_straggler
Star at the centre of the Solar System
Iben, Icko Jnr. (November 1965). "Stellar Evolution. II. The Evolution of a 3 M☉ Star from the Main Sequence Through Core Helium Burning". The Astrophysical
Sun
Coming together of two stars
A stellar collision is the coming together of two stars caused by stellar dynamics within a star cluster, or by the orbital decay of a binary star due
Stellar_collision
Collapsed core of a massive star
the main sequence, stellar nucleosynthesis produces an iron-rich core. When all nuclear fuel in the core has been exhausted, the core must be supported
Neutron_star
Stars with a supergiant luminosity class with a spectral type of K or M
(RSGs) are stars with a supergiant luminosity class (Yerkes class I) and a stellar classification K or M. They are the largest stars in the universe in terms
Red_supergiant
Hot, luminous star with a spectral type of A9 or earlier
unusual stellar interiors (such as hotter blue supergiants having oversized hydrogen-fusing cores and cooler ones having undersized helium-fusing cores) may
Blue_supergiant
Dim, low mass stars on the main sequence
definition is synonymous with stellar M dwarfs, yielding a maximum temperature of 3,900 K and 0.6 M☉. Another includes all stellar M-type main-sequence and
Red_dwarf
Hypothetical hybrid star type
red supergiant. It is possible to detect pre-existing TŻOs with current LIGO detectors; the neutron star core would emit a continuous wave. It has been
Thorne–Żytkow_object
Study of oscillations in stars
Asteroseismology is closely related to helioseismology, the study of stellar pulsation specifically in the Sun. Though both are based on the same underlying
Asteroseismology
Luminosity–temperature relationship in stars
relationship obeyed by infant stars of less than 3 M☉ in the pre-main-sequence phase (PMS phase) of stellar evolution. It is named after Japanese astrophysicist
Hayashi_track
Subfield of astronomy
Stellar pulsation – Oscillations revealing stellar interiors via asteroseismology. Frequency separation – Asteroseismic diagnostic of stellar core rotation
Outline_of_astrophysics
Class of young variable stars
obeyed by infant stars of less than 3 solar masses (M☉) in the pre-main-sequence phase of stellar evolution. It ends when a star of 0.5 M☉ or larger develops
T_Tauri_star
Branch of astrophysics
Stellar dynamics is the branch of astrophysics which describes in a statistical way the collective motions of stars subject to their mutual gravity. The
Stellar_dynamics
Region of a star
In a radiation zone, energy is transported by radiation and conduction. Stellar convection consists of mass movement of plasma within the star which usually
Convection_zone
Stellar classification
A K-type main-sequence star is a main-sequence (core hydrogen-burning) star of spectral type K. The spectral luminosity class is V. These stars are intermediate
K-type_main-sequence_star
Ejecta from the Sun's corona
are always present in the pre-eruption structure or whether they are created during the eruption from a strongly sheared core field (see § Initiation)
Coronal_mass_ejection
Supernova at least ten times more luminous than a standard supernova
supernova (SLSN, plural superluminous supernovae or SLSNe) is a type of stellar explosion with a luminosity 10 or more times higher than that of standard
Superluminous_supernova
Astronomical category of stars
observed types of star: Binary stars with highly variable emission and stellar spectral type Fe a blue supergiant with a forest of forbidden FeII lines
Iron_star
Angular motion of a star about its axis
Stellar rotation is the angular motion of a star about its axis. The rate of rotation can be measured from the spectrum of the star, or by timing the
Stellar_rotation
Curve on the Hertzsprung-Russell diagram representing stars of a particular age
In stellar evolution, an isochrone is a curve on the Hertzsprung-Russell diagram, representing a population of stars of the same age but with different
Stellar_isochrone
Part of a star
not gravitationally bound to the star core. Usually circumstellar envelopes are formed from the dense stellar wind, or they are present before the formation
Circumstellar_envelope
Stellar classification
An F-type main-sequence star is a main-sequence, core-hydrogen-fusing star of spectral type F. The spectral luminosity class is V. They have from around
F-type_main-sequence_star
Stellar classification
An A-type main-sequence star is a main-sequence (core hydrogen burning) star of spectral type A. The spectral luminosity class is V. These stars have spectra
A-type_main-sequence_star
Explosion of a star 8 to 45 times the mass of the Sun
situation known as stellar or hydrostatic equilibrium. The helium produced in the core accumulates there. Temperatures in the core are not yet high enough
Type_II_supernova
Multiple star system in the constellation Carina
HD 97950, is the central core of a super star cluster within the NGC 3603 H II region (similar to R136 within the Tarantula Nebula). It was catalogued
HD_97950
Main-sequence star of spectral type O
about −5.8 (eqv. 18,000 times brighter than the sun). Their light-driven stellar winds have a terminal velocity around 2,000 km/s. The most luminous class O
O-type_main-sequence_star
Astronomical object without the mass to sustain hydrogen fusion
enough mass to fuse hydrogen and helium, hence do not undergo the usual stellar evolution that limits the lifetime of stars. A substellar object with a
Substellar_object
Stellar phenomenon
Starspots are stellar phenomena, so-named by analogy with sunspots. Spots as small as sunspots have not been detected on other stars, as they would cause
Starspot
Type of interstellar cloud
A molecular cloud—sometimes called a stellar nursery if star formation is occurring within—is a type of interstellar cloud of which the density and size
Molecular_cloud
Type of star that is massive and luminous
blue, yellow, and red supergiants serve as an indicator of the speed of stellar evolution and are used as a powerful test of models of the evolution of
Supergiant
Process of creating new atomic nuclei from existing nucleons
Stars fuse light elements to heavier ones in their cores, giving off energy in the process known as stellar nucleosynthesis. Nuclear fusion reactions create
Nucleosynthesis
Production of the elements in a supernova explosion
the remainder of stellar nucleosynthesis occurs, however, in stars that are massive enough to end as core collapse supernovae. In the pre-supernova massive
Supernova_nucleosynthesis
Nuclear explosion in a white dwarf star
velocity Kilonova – Aftermath of a neutron star merger Micronova – Explosive stellar phenomenon about one millionth the strength of a classical nova Superluminous
Nova
Point in stellar evolution
eventually run out of fuel. Once all the available hydrogen has been fused stellar nucleosynthesis stops, and the remaining helium slowly cools by radiation
Main_sequence_turnoff
Young stars of spectral types A and B
than F0 (in order to exclude T Tauri stars), Balmer emission lines in the stellar spectrum (in order to be similar to T Tauri stars), Projected location
Herbig_Ae/Be_star
Star not gravitationally bound to any galaxy
Collectively, intergalactic stars are referred to as the intracluster stellar population, or IC population for short, in the scientific literature. The
Intergalactic_star
Empirical function in astronomy
and the origin of the stellar IMF. Herschel observations of the California giant molecular cloud show that both the prestellar core mass function (CMF)
Initial_mass_function
Boundary between solar corona and wind
separating a star's corona from the stellar wind defined as where the coronal plasma's Alfvén speed and the large-scale stellar wind speed are equal. It is named
Alfvén_surface
Relative abundance of heavy elements in a star or other astronomical object
result of stellar nucleosynthesis. The majority of elements that are heavier than hydrogen and helium in the Universe are formed in the cores of stars
Metallicity
Stage of stellar evolution
In the field of stellar evolution, a blue loop is a stage in the life of an evolved star where it changes from a cool star to a hotter one before cooling
Blue_loop
Light from the stars
telescopes is the basis for many fields of astronomy, including photometry and stellar spectroscopy. Hipparchus did not have a telescope or any instrument that
Starlight
Region of an astronomical diagram
the right of the brighter Cepheids (at lower temperatures), since their stellar pulsations are attributed to the same mechanism. The Hertzsprung–Russell
Instability_strip
Astronomical object capable of nuclear fusion
Objects are considered "stellar" when they are about 75 MJ, when their gravitational contraction is halted by the heat generated by core fusion, establishing
Fusor_(astronomy)
travel, tourism, insurance
PRE STELLAR-CORE
PRE STELLAR-CORE
PRE STELLAR-CORE
PRE STELLAR-CORE
PRE STELLAR-CORE
PRE STELLAR-CORE
PRE STELLAR-CORE
PRE STELLAR-CORE
PRE STELLAR-CORE
travel, tourism, insurance