Table of Contents
42 relations: Asymptotic giant branch, B-type main-sequence star, Beehive Cluster, Classical Cepheid variable, CNO cycle, Convection zone, Degenerate matter, Dredge-up, Giant star, Helium, Helium flash, Hertzsprung gap, Hertzsprung–Russell diagram, Horizontal branch, Hydrogen, Instability strip, Long-period variable star, Magellanic Clouds, Main sequence, Metallicity, Microlensing Observations in Astrophysics, Milky Way, Mira, Mira variable, Normal mode, Optical Gravitational Lensing Experiment, Overtone, Period-luminosity relation, Red clump, Red giant, Schönberg–Chandrasekhar limit, Semiregular variable star, Slow irregular variable, Solar mass, Solar-like oscillations, Stellar evolution, Stochastic, Subgiant, Thermal equilibrium, Tip of the red-giant branch, Variable star, White dwarf.
- Hertzsprung–Russell classifications
- Red giants
Asymptotic giant branch
The asymptotic giant branch (AGB) is a region of the Hertzsprung–Russell diagram populated by evolved cool luminous stars.
See Red-giant branch and Asymptotic giant branch
B-type main-sequence star
A B-type main-sequence star (B V) is a main-sequence (hydrogen-burning) star of spectral type B and luminosity class V. These stars have from 2 to 16 times the mass of the Sun and surface temperatures between 10,000 and 30,000 K. B-type stars are extremely luminous and blue.
See Red-giant branch and B-type main-sequence star
Beehive Cluster
The Beehive Cluster (also known as Praesepe (Latin for "manger", "cot" or "crib"), M44, NGC 2632, or Cr 189), is an open cluster in the constellation Cancer.
See Red-giant branch and Beehive Cluster
Classical Cepheid variable
Classical Cepheids are a type of Cepheid variable star.
See Red-giant branch and Classical Cepheid variable
CNO cycle
The CNO cycle (for carbon–nitrogen–oxygen; sometimes called Bethe–Weizsäcker cycle after Hans Albrecht Bethe and Carl Friedrich von Weizsäcker) is one of the two known sets of fusion reactions by which stars convert hydrogen to helium, the other being the proton–proton chain reaction (p–p cycle), which is more efficient at the Sun's core temperature.
See Red-giant branch and CNO cycle
Convection zone
A convection zone, convective zone or convective region of a star is a layer which is unstable due to convection.
See Red-giant branch and Convection zone
Degenerate matter
Degenerate matter occurs when the Pauli exclusion principle significantly alters a state of matter at low temperature.
See Red-giant branch and Degenerate matter
Dredge-up
A dredge-up is any one of several stages in the evolution of some stars.
See Red-giant branch and Dredge-up
Giant star
A giant star has a substantially larger radius and luminosity than a main-sequence (or dwarf) star of the same surface temperature.
See Red-giant branch and Giant star
Helium
Helium (from lit) is a chemical element; it has symbol He and atomic number 2.
See Red-giant branch and Helium
Helium flash
A helium flash is a very brief thermal runaway nuclear fusion of large quantities of helium into carbon through the triple-alpha process in the core of low-mass stars (between 0.8 solar masses and 2.0) during their red giant phase.
See Red-giant branch and Helium flash
Hertzsprung gap
The Hertzsprung gap is a feature of the Hertzsprung–Russell diagram for a star cluster. Red-giant branch and Hertzsprung gap are Hertzsprung–Russell classifications.
See Red-giant branch and Hertzsprung gap
Hertzsprung–Russell diagram
The Hertzsprung–Russell diagram (abbreviated as H–R diagram, HR diagram or HRD) is a scatter plot of stars showing the relationship between the stars' absolute magnitudes or luminosities and their stellar classifications or effective temperatures. Red-giant branch and Hertzsprung–Russell diagram are Hertzsprung–Russell classifications.
See Red-giant branch and Hertzsprung–Russell diagram
Horizontal branch
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.
See Red-giant branch and Horizontal branch
Hydrogen
Hydrogen is a chemical element; it has symbol H and atomic number 1.
See Red-giant branch and Hydrogen
Instability strip
The unqualified term instability strip usually refers to a region of the Hertzsprung–Russell diagram largely occupied by several related classes of pulsating variable stars: Delta Scuti variables, SX Phoenicis variables, and rapidly oscillating Ap stars (roAps) near the main sequence; RR Lyrae variables where it intersects the horizontal branch; and the Cepheid variables where it crosses the supergiants. Red-giant branch and instability strip are Hertzsprung–Russell classifications.
See Red-giant branch and Instability strip
Long-period variable star
The descriptive term long-period variable star refers to various groups of cool luminous pulsating variable stars.
See Red-giant branch and Long-period variable star
Magellanic Clouds
The Magellanic Clouds (Magellanic system or Nubeculae Magellani) are two irregular dwarf galaxies in the southern celestial hemisphere.
See Red-giant branch and Magellanic Clouds
Main sequence
In astronomy, the main sequence is a classification of stars which appear on plots of stellar color versus brightness as a continuous and distinctive band.
See Red-giant branch and Main sequence
Metallicity
In astronomy, metallicity is the abundance of elements present in an object that are heavier than hydrogen and helium.
See Red-giant branch and Metallicity
Microlensing Observations in Astrophysics
Microlensing Observations in Astrophysics (MOA) is a collaborative project between researchers in New Zealand and Japan, led by Professor Yasushi Muraki of Nagoya University.
See Red-giant branch and Microlensing Observations in Astrophysics
Milky Way
The Milky Way is the galaxy that includes the Solar System, with the name describing the galaxy's appearance from Earth: a hazy band of light seen in the night sky formed from stars that cannot be individually distinguished by the naked eye.
See Red-giant branch and Milky Way
Mira
Mira, designation Omicron Ceti (ο Ceti, abbreviated Omicron Cet, ο Cet), is a red-giant star estimated to be 200–300 light-years from the Sun in the constellation Cetus.
Mira variable
Mira variables (named for the prototype star Mira) are a class of pulsating stars characterized by very red colours, pulsation periods longer than 100 days, and amplitudes greater than one magnitude in infrared and 2.5 magnitude at visual wavelengths.
See Red-giant branch and Mira variable
Normal mode
A normal mode of a dynamical system is a pattern of motion in which all parts of the system move sinusoidally with the same frequency and with a fixed phase relation.
See Red-giant branch and Normal mode
Optical Gravitational Lensing Experiment
The Optical Gravitational Lensing Experiment (OGLE) is a Polish astronomical project based at the University of Warsaw that runs a long-term variability sky survey (1992–present).
See Red-giant branch and Optical Gravitational Lensing Experiment
Overtone
An overtone is any resonant frequency above the fundamental frequency of a sound.
See Red-giant branch and Overtone
Period-luminosity relation
In astronomy, a period-luminosity relation is a relationship linking the luminosity of pulsating variable stars with their pulsation period.
See Red-giant branch and Period-luminosity relation
Red clump
The red clump is a clustering of red giants in the Hertzsprung–Russell diagram at around 5,000 K and absolute magnitude (MV) +0.5, slightly hotter than most red-giant-branch stars of the same luminosity. Red-giant branch and red clump are red giants.
See Red-giant branch and Red clump
Red giant
A red giant is a luminous giant star of low or intermediate mass (roughly 0.3–8 solar masses) in a late phase of stellar evolution. Red-giant branch and red giant are red giants.
See Red-giant branch and Red giant
Schönberg–Chandrasekhar limit
In stellar astrophysics, the Schönberg–Chandrasekhar limit is the maximum mass of a non-fusing, isothermal core that can support an enclosing envelope.
See Red-giant branch and Schönberg–Chandrasekhar limit
Semiregular variable star
In astronomy, a semiregular variable star, a type of variable star, is a giant or supergiant of intermediate and late (cooler) spectral type showing considerable periodicity in its light changes, accompanied or sometimes interrupted by various irregularities.
See Red-giant branch and Semiregular variable star
Slow irregular variable
A slow irregular variable (ascribed the GCVS types L, LB and LC) is a variable star that exhibit no or very poorly defined periodicity in their slowly changing light emissions.
See Red-giant branch and Slow irregular variable
Solar mass
The solar mass is a standard unit of mass in astronomy, equal to approximately.
See Red-giant branch and Solar mass
Solar-like oscillations
Solar-like oscillations are oscillations in stars that are excited in the same way as those in the Sun, namely by turbulent convection in its outer layers.
See Red-giant branch and Solar-like oscillations
Stellar evolution
Stellar evolution is the process by which a star changes over the course of its lifetime and how it can lead to the creation of a new star.
See Red-giant branch and Stellar evolution
Stochastic
Stochastic refers to the property of being well-described by a random probability distribution.
See Red-giant branch and Stochastic
Subgiant
A subgiant is a star that is brighter than a normal main-sequence star of the same spectral class, but not as bright as giant stars.
See Red-giant branch and Subgiant
Thermal equilibrium
Two physical systems are in thermal equilibrium if there is no net flow of thermal energy between them when they are connected by a path permeable to heat.
See Red-giant branch and Thermal equilibrium
Tip of the red-giant branch
Tip of the red-giant branch (TRGB) is a primary distance indicator used in astronomy. Red-giant branch and Tip of the red-giant branch are red giants.
See Red-giant branch and Tip of the red-giant branch
Variable star
A variable star is a star whose brightness as seen from Earth (its apparent magnitude) changes with time.
See Red-giant branch and Variable star
White dwarf
A white dwarf is a stellar core remnant composed mostly of electron-degenerate matter.
See Red-giant branch and White dwarf
See also
Hertzsprung–Russell classifications
- Blue loop
- Bright giants
- Giant stars
- Hayashi track
- Henyey track
- Hertzsprung gap
- Hertzsprung–Russell diagram
- Hess diagram
- Hypergiants
- Instability strip
- Main-sequence stars
- Pre-main-sequence stars
- Red dwarfs
- Red-giant branch
- Stellar birthline
- Stellar classification
- Subdwarfs
- Supergiants
- White dwarfs
Red giants
- Carbon stars
- Gaia BH2
- HD 34266
- RT Virginis
- Red clump
- Red giant
- Red-giant branch
- Symbiotic binary
- Thorne–Żytkow object
- Tip of the red-giant branch
References
Also known as First giant branch, Red giant branch, Red giant branch stars.