X Cancri

X Cancri is a variable star in the northern constellation of Cancer. ^[1]

18 relations: Asymptotic giant branch, Cancer (constellation), Carbon star, Chi Cancri, Constellation, Ecliptic, Fourier analysis, Light-year, Occultation, Radial velocity, Red giant, S-type star, Semiregular variable star, Stellar atmosphere, Stellar parallax, Swan band, Variable star, Very-long-baseline interferometry.
Carbon stars

Asymptotic giant branch

The asymptotic giant branch (AGB) is a region of the Hertzsprung–Russell diagram populated by evolved cool luminous stars. X Cancri and asymptotic giant branch are asymptotic-giant-branch stars.

See X Cancri and Asymptotic giant branch

Cancer (constellation)

Cancer is one of the twelve constellations of the zodiac and is located in the Northern celestial hemisphere.

See X Cancri and Cancer (constellation)

Carbon star

A carbon star (C-type star) is typically an asymptotic giant branch star, a luminous red giant, whose atmosphere contains more carbon than oxygen. X Cancri and carbon star are carbon stars.

See X Cancri and Carbon star

Chi Cancri, Latinized from χ Cancri, is a candidate astrometric binary star system in the northern zodiac constellation of Cancer. X Cancri and Chi Cancri are bright Star Catalogue objects, Cancer (constellation), Henry Draper Catalogue objects and Hipparcos objects.

See X Cancri and Chi Cancri

Constellation

A constellation is an area on the celestial sphere in which a group of visible stars forms a perceived pattern or outline, typically representing an animal, mythological subject, or inanimate object.

See X Cancri and Constellation

Ecliptic

The ecliptic or ecliptic plane is the orbital plane of Earth around the Sun.

See X Cancri and Ecliptic

Fourier analysis

In mathematics, Fourier analysis is the study of the way general functions may be represented or approximated by sums of simpler trigonometric functions.

See X Cancri and Fourier analysis

Light-year

A light-year, alternatively spelled light year (ly or lyr), is a unit of length used to express astronomical distances and is equal to exactly 9,460,730,472,580.8 km (Scientific notation: 9.4607304725808 × 1012 km), which is approximately 5.88 trillion mi.

See X Cancri and Light-year

Occultation

An occultation is an event that occurs when one object is hidden from the observer by another object that passes between them.

See X Cancri and Occultation

Radial velocity

The radial velocity or line-of-sight velocity of a target with respect to an observer is the rate of change of the vector displacement between the two points.

See X Cancri and Radial velocity

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.

See X Cancri and Red giant

S-type star

An S-type star (or just S star) is a cool giant with approximately equal quantities of carbon and oxygen in its atmosphere.

See X Cancri and S-type star

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. X Cancri and semiregular variable star are semiregular variable stars.

See X Cancri and Semiregular variable star

Stellar atmosphere

The stellar atmosphere is the outer region of the volume of a star, lying above the stellar core, radiation zone and convection zone.

See X Cancri and Stellar atmosphere

Stellar parallax

Stellar parallax is the apparent shift of position (parallax) of any nearby star (or other object) against the background of distant stars.

See X Cancri and Stellar parallax

Swan band

Swan bands are a characteristic of the spectra of carbon stars, comets and of burning hydrocarbon fuels.

See X Cancri and Swan band

Variable star

A variable star is a star whose brightness as seen from Earth (its apparent magnitude) changes with time.

See X Cancri and Variable star

Very-long-baseline interferometry

Very-long-baseline interferometry (VLBI) is a type of astronomical interferometry used in radio astronomy.

See X Cancri and Very-long-baseline interferometry

References

[1] https://en.wikipedia.org/wiki/X_Cancri

Also known as X Cnc.

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