66 relations: Amateur astronomy, Apparent magnitude, Astrophysical maser, Asymptotic giant branch, Chi Cygni, CW Leonis, Dredge-up, Dust, Helium, Hydrogen, IK Tauri, Infrared, Infrared Optical Telescope Array, LL Pegasi, Long-period variable star, Luminosity, Mira, Mira (given name), Parsec, Planetary nebula, R Andromedae, R Aquarii, R Aquilae, R Aurigae, R Boötis, R Cancri, R Canum Venaticorum, R Capricorni, R Carinae, R Cassiopeiae, R Centauri, R Cygni, R Doradus, R Geminorum, R Horologii, R Hydrae, R Leonis, R Leonis Minoris, R Leporis, R Normae, R Octantis, R Reticuli, R Serpentis, R Virginis, Red giant, S Boötis, S Carinae, S Coronae Borealis, S Orionis, S Pictoris, ..., S Virginis, Semiregular variable star, Solar mass, Southern Crab Nebula, Stellar evolution, Sun, T Cephei, T Normae, TX Camelopardalis, U Herculis, U Orionis, V Coronae Borealis, Variable star, W Aquilae, W Hydrae, White dwarf. Expand index (16 more) » « Shrink index
Amateur astronomy is a hobby whose participants enjoy observing or imaging celestial objects in the sky using the unaided eye, binoculars, or telescopes.
The apparent magnitude of a celestial object is a number that is a measure of its brightness as seen by an observer on Earth.
An astrophysical maser is a naturally occurring source of stimulated spectral line emission, typically in the microwave portion of the electromagnetic spectrum.
The asymptotic giant branch (AGB) is a region of the Hertzsprung–Russell diagram populated by evolved cool luminous stars.
Chi Cygni (χ Cyg, χ Cygni) is a variable star of the Mira type in the constellation Cygnus, and also an S-type star.
IRC +10216 or CW Leonis is a well-studied carbon star that is embedded in a thick dust envelope. It was first discovered in 1969 by a group of astronomers led by Eric Becklin, based upon infrared observations made with the Caltech Infrared Telescope at Mount Wilson Observatory. Its energy is emitted mostly at infrared wavelengths. At a wavelength of 5 μm, it was found to have the highest flux of any object outside the Solar System.
A dredge-up is a period in the evolution of a star where a surface convection zone extends down to the layers where material has undergone nuclear fusion.
Dust are fine particles of matter.
Helium (from lit) is a chemical element with symbol He and atomic number 2.
Hydrogen is a chemical element with symbol H and atomic number 1.
IK Tauri is a Mira variable star located about from the Sun in the zodiac constellation of Taurus.
Infrared radiation (IR) is electromagnetic radiation (EMR) with longer wavelengths than those of visible light, and is therefore generally invisible to the human eye (although IR at wavelengths up to 1050 nm from specially pulsed lasers can be seen by humans under certain conditions). It is sometimes called infrared light.
The Infrared Optical Telescope Array (IOTA) was a stellar interferometer array.
LL Pegasi (AFGL 3068) is a Mira variable star surrounded by a pinwheel-shaped nebula, IRAS 23166+1655, thought to be a preplanetary nebula.
The descriptive term long-period variable star refers to various groups of cool luminous pulsating variable stars.
In astronomy, luminosity is the total amount of energy emitted per unit of time by a star, galaxy, or other astronomical object.
Mira, alternatively designated Omicron Ceti (ο Ceti, abbreviated Omicron Cet, ο Cet) is a red giant star estimated to be 200–400 light years from the Sun in the constellation of Cetus.
Mira is a feminine given name with varying meanings.
The parsec (symbol: pc) is a unit of length used to measure large distances to astronomical objects outside the Solar System.
A planetary nebula, abbreviated as PN or plural PNe, is a type of emission nebula consisting of an expanding, glowing shell of ionized gas ejected from red giant stars late in their lives.
R Andromedae (R And) is a Mira-type variable star in the constellation Andromeda.
R Aquarii (R Aqr) is a variable star in the constellation Aquarius.
R Aquilae is a Mira variable in the constellation Aquila.
R Aurigae (R Aur) is a M-type giant star in the constellation of Auriga.
R Boötis is a Mira variable in the constellation Boötes.
R Cancri is a Mira variable in the constellation Cancer.
R Canum Venaticorum is a Mira variable star in the constellation Canes Venatici.
R Capricorni (R Cap) is a star in the constellation of Capricornus.
R Carinae is a star in the constellation Carina.
R Cassiopeiae (R Cas) is a star in the constellation Cassiopeia.
R Centauri (R Cen) is a Mira variable star in the constellation Centaurus.
R Cygni is a variable star of the Mira type in the constellation Cygnus.
R Doradus (HD 29712 or P Doradus) is the name of a red giant Mira variable star in the far-southern constellation Dorado, although visually it appears more closely associated with the constellation Reticulum.
R Geminorum (R Gem) is a Mira variable and technetium star in the constellation Gemini.
R Horologii (also known as HD 18242) is a red giant star approximately 700 light-years away in the constellation Horologium.
R Hydrae, also known as R Hya, is a Mira-type variable star in the constellation Hydra.
R Leonis is a red giant Mira-type variable star located approximately 300 light years away in the constellation Leo.
R Leonis Minoris (R LMi) is a Mira variable type star in the constellation Leo Minor.
R Leporis (R Lep), sometimes called Hind's Crimson Star, is a well-known variable star in the constellation Lepus, near its border with Eridanus.
R Normae is a Mira variable star located near Eta Normae in the southern constellation of Norma.
R Octantis is a Mira variable star located in the southern constellation of Octans.
R Reticuli (R Ret) is a Mira variable star in the constellation Reticulum.
R Serpentis (R Ser) is a Mira variable type star in the constellation Serpens.
R Virginis is a Mira variable in the constellation Virgo.
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.
S Boötis is a Mira variable in the constellation Boötes.
The Bayer designations S Carinae and s Carinae are distinct.
S Coronae Borealis (S CrB) is a Mira variable star in the constellation Corona Borealis.
S Orionis is a asymptotic giant branch star in the constellation Orion, approximately away.
S Pictoris is a Mira variable-type star in the constellation Pictor.
S Virginis is a Mira-type variable star in the constellation Virgo.
Semiregular variable stars are giants or supergiants of intermediate and late spectral type showing considerable periodicity in their light changes, accompanied or sometimes interrupted by various irregularities.
The solar mass is a standard unit of mass in astronomy, equal to approximately.
The Southern Crab Nebula or Hen 2-104 is a nebula in the constellation Centaurus.
Stellar evolution is the process by which a star changes over the course of time.
The Sun is the star at the center of the Solar System.
T Cephei is a Mira variable star in the constellation Cepheus.
T Normae is a Mira variable star.
TX Camelopardalis (abbreviated TX Cam) is a Mira-type variable star in the constellation Camelopardalis.
The Bayer designations u Herculis and U Herculis are distinct.
U Orionis (abbreviated U Ori) is a Mira-type variable star in the constellation Orion.
V Coronae Borealis (V CrB) is a Mira-type long period variable star and carbon star in the constellation Corona Borealis.
A variable star is a star whose brightness as seen from Earth (its apparent magnitude) fluctuates.
W Aquilae (W Aql / SAO 143184 / GC 2525) is a variable star in the constellation of Aquila.
W Hydrae is a Mira-type variable star in the constellation Hydra.
A white dwarf, also called a degenerate dwarf, is a stellar core remnant composed mostly of electron-degenerate matter.