AI & ChatGPT searches , social queries for W URSAE-MAJORIS-VARIABLE
Search references for W URSAE-MAJORIS-VARIABLE. Phrases containing W URSAE-MAJORIS-VARIABLE
See searches and references containing W URSAE-MAJORIS-VARIABLE!
Search references for W URSAE-MAJORIS-VARIABLE. Phrases containing W URSAE-MAJORIS-VARIABLE
See searches and references containing W URSAE-MAJORIS-VARIABLE!W URSAE-MAJORIS-VARIABLE
Type of variable stellar binary
A W Ursae Majoris variable, also known as a low mass contact binary, is a type of eclipsing binary variable star. These stars are close binaries of spectral
W_Ursae_Majoris_variable
Star in the constellation Ursa Major
W Ursae Majoris (W UMa) is the variable star designation for a binary star system in the northern constellation of Ursa Major. It has an apparent visual
W_Ursae_Majoris
Star in the constellation Ursa Major
Ursae Majoris is a variable star in the northern circumpolar constellation of Ursa Major, located 104.7 light-years from the Sun. It has the variable
24_Ursae_Majoris
Variable star in the constellation Ursa Major
DW Ursae Majoris is an eclipsing binary star system in the northern circumpolar constellation of Ursa Major, abbreviated DW UMa. It is a cataclysmic variable
DW_Ursae_Majoris
Variable star in the constellation Ursa Major
Ursae Majoris is an Algol type binary star system in the northern circumpolar constellation of Ursa Major. It is classified as a nova-like variable star
UX_Ursae_Majoris
Star in the constellation Ursa Major
Nu Ursae Majoris (ν Ursae Majoris, abbreviated Nu UMa, ν UMa), formally named Alula Borealis /əˈluːlə bɒriˈælɪs/, is a double star in the northern circumpolar
Nu_Ursae_Majoris
Binary star in the constellation Ursa Major
constellation of Ursa Major. It is formally designated Alpha Ursae Majoris, Latinised from α Ursae Majoris, Despite being designated "α" (alpha), it is the second-brightest
Dubhe
Eclipsing binary star system in the constellation of Ursa Major
XY Ursae Majoris is a short period binary star system in the northern circumpolar constellation of Ursa Major. It is an eclipsing binary with a baseline
XY_Ursae_Majoris
Variable star in the constellation Ursa Major
AW Ursae Majoris is a binary star system in the northern circumpolar constellation of Ursa Major, abbreviated AW UMa. It is an A-type W Ursae Majoris variable
AW_Ursae_Majoris
Star in the constellation Ursa Major
Pi1 Ursae Majoris (Pi1 UMa, π1 Ursae Majoris, π1 UMa) is a yellow G-type main sequence dwarf with a mean apparent magnitude of +5.63. It is approximately
Pi1_Ursae_Majoris
Variable star in the constellation Ursa Major
SW Ursae Majoris is a cataclysmic binary star system in the northern circumpolar constellation of Ursa Major, abbreviated SW UMa. During quiescence it
SW_Ursae_Majoris
Variable star in the constellation Ursa Major
BE Ursae Majoris is a binary star system in the northern circumpolar constellation of Ursa Major, abbreviated BE UMa. The two components are an unusual
BE_Ursae_Majoris
Star in the constellation Ursa Major
18 Ursae Majoris, or e Ursae Majoris, is a single star in the northern circumpolar constellation of Ursa Major. It is faintly visible to the naked eye
18_Ursae_Majoris
Variable binary star system in the constellation Ursa Major
ER Ursae Majoris is a variable star in the northern circumpolar constellation of Ursa Major, abbreviated ER UMa. It is a prototype system for a subclass
ER_Ursae_Majoris
Variable star in the constellation Ursa Major
AE Ursae Majoris is a star in the northern circumpolar constellation of Ursa Major, abbreviated AE UMa. It is a variable star that ranges in brightness
AE_Ursae_Majoris
Binary star in the constellation Ursa Major
Upsilon Ursae Majoris, Latinized from υ Ursae Majoris, is a binary star in the northern circumpolar constellation of Ursa Major. It is visible to the
Upsilon_Ursae_Majoris
Variable star in the constellation Ursa Major
CQ Ursae Majoris is a variable star in the northern circumpolar constellation of Ursa Major, abbreviated CQ UMa. It is sometimes identified as HR 5153
CQ_Ursae_Majoris
Star in the constellation Ursa Major
Merak /ˈmɪəræk/, also called Beta Ursae Majoris (β Ursae Majoris, abbreviated Beta UMa, β UMa), is a star in the northern constellation of Ursa Major.
Merak_(star)
Star in the constellation Ursa Major
23 Ursae Majoris, or 23 UMa, is a binary star system in the constellation Ursa Major, located is approximately 77.7 light years from the Sun. It has the
23_Ursae_Majoris
Binary star in the constellation Ursa Major
Sigma2 Ursae Majoris (σ2 Ursae Majoris, σ2 UMa) is a binary star in the constellation of Ursa Major. Parallax measurements made by the Hipparcos spacecraft
Sigma2_Ursae_Majoris
Variable star in the constellation Ursa Major
AN Ursae Majoris is a binary star system in the northern circumpolar constellation of Ursa Major. It is a variable star, with AN Ursae Majoris being the
AN_Ursae_Majoris
Star whose brightness fluctuates, as seen from Earth
standstills are seen, part way between maximum and minimum brightness. SU Ursae Majoris stars, which undergo both frequent small outbursts, and rarer but larger
Variable_star
Eclipsing binary star system in the constellation of Ursa Major
TX Ursae Majoris is an eclipsing binary star system in the northern circumpolar constellation of Ursa Major. With a combined apparent visual magnitude
TX_Ursae_Majoris
Variable star system in the constellation Ursa Major
VV Ursae Majoris is a binary star system in the northern circumpolar constellation of Ursa Major, abbreviated VV UMa. It is a variable star system with
VV_Ursae_Majoris
Star in the constellation Ursa Major
Megrez /ˈmiːɡrɛz/, also called Delta Ursae Majoris (δ Ursae Majoris, abbreviated Delta UMa, δ UMa), is a star in the northern constellation of Ursa Major
Megrez
Star in the constellation Ursa Major
Alkaid /ælˈkeɪd/, also called Eta Ursae Majoris (Latinised from η Ursae Majoris, abbreviated Eta UMa, η UMa), is a star in the constellation of Ursa Major
Alkaid
Variable star in the constellation Ursa Major
SU Ursae Majoris, or SU UMa, is a close binary star in the northern circumpolar constellation of Ursa Major. It is a periodic cataclysmic variable that
SU_Ursae_Majoris
Star in the constellation Ursa Major
Chi Ursae Majoris or χ Ursae Majoris, formally named Taiyangshou /ˌtaɪˌjæŋˈʃoʊ/, is a single star in the northern circumpolar constellation of Ursa Major
Chi_Ursae_Majoris
Variable star in the constellation Ursa Major
DM Ursae Majoris is a binary star system in the northern circumpolar constellation of Ursa Major, abbreviated DM UMa. It is sometimes identified by the
DM_Ursae_Majoris
Binary star system in the constellation Ursa Major
78 Ursae Majoris is a binary star system in the northern circumpolar constellation of Ursa Major. It is visible to the naked eye as a faint point of light
78_Ursae_Majoris
Eclipsing contact binary in Holmberg IX
Holmberg IX V1, also known as EQ J095737+690211 is a W Ursae Majoris type eclipsing contact binary star system in the constellation of Ursa Major. The
Holmberg_IX_V1
Variable star
TU Ursae Majoris is a variable star in the northern circumpolar constellation of Ursa Major. It is classified as a Bailey-type 'ab' RR Lyrae variable with
TU_Ursae_Majoris
Constellation in the northern sky
steps". W Ursae Majoris is the prototype of a class of contact binary variable stars, and ranges between magnitudes 7.75 and 8.48. 47 Ursae Majoris is a Sun-like
Ursa_Major
Dwarf Nova in the constellation Ursa Major
BZ Ursae Majoris is a dwarf nova star system in the northern circumpolar constellation of Ursa Major. It consists of a white dwarf primary in a close
BZ_Ursae_Majoris
Solitary star in the constellation Ursa Major
Sigma1 Ursae Majoris (σ1 UMa) is the Bayer designation for a solitary star in the northern circumpolar constellation of Ursa Major. With an apparent visual
Sigma1_Ursae_Majoris
Star in the Ursa Major constellation
61 Ursae Majoris, abbreviated 61 UMa, is a single star in the northern circumpolar constellation of Ursa Major. It has a yellow-orange hue and is dimly
61_Ursae_Majoris
Quintuple star system in the constellation Ursa Major
78+533859.5 (abbreviated as J093010), also known as V441 Ursae Majoris and V442 Ursae Majoris is a quintuple star system located in the constellation Ursa
1SWASP_J093010.78+533859.5
Star system in the constellation Ursa Major
Theta Ursae Majoris (Theta UMa, θ Ursae Majoris, θ UMa) is a suspected spectroscopic binary star system in the northern circumpolar constellation of Ursa
Theta_Ursae_Majoris
Binary star system whose component stars are very close
eclipsing contact binaries are known as W Ursae Majoris variables, after their archetype star, W Ursae Majoris. In a contact binary, both stars have filled
Contact_binary
Constellation in the northern celestial hemisphere
also be found by following a line through the two stars—Alpha and Beta Ursae Majoris, popularly called the Pointers—that form the end of the "bowl" of the
Ursa_Minor
Constellation in the southern celestial hemisphere
around 4.1. Epsilon Coronae Australis is the brightest example of a W Ursae Majoris variable in the southern sky. Lying alongside the Milky Way, Corona Australis
Corona_Australis
Constellation in the northern celestial hemisphere
itself an eclipsing variable star with a range of 0.6 magnitudes; its orbital period is 6.4 hours. It is a W Ursae Majoris variable that ranges in magnitude
Boötes
Variable star in the constellation Sextans
are separated by 0.50 arcseconds. The brighter component is a W Ursae Majoris variable eclipsing contact binary star system, whose two component stars
Y_Sextantis
Star in the constellation Antlia
S Antliae is a W Ursae Majoris-type eclipsing binary star in Antlia. S Antiliae is classed as an A-type W Ursae Majoris variable, since the primary is
S_Antliae
+55° 57′ 35.4″ 1.77 −0.21 81 A0p Alioth; brown dwarf companion?; α2 CVn variable Dubhe α 50 95689 54061 11h 03m 43.84s +61° 45′ 04.0″ 1.79 −1.08 124 K0III
List_of_stars_in_Ursa_Major
Variable star in the constellation Cassiopeia
constellation of Cassiopeia. It is classified as an overcontact binary of the W Ursae Majoris (W UMa) type. It has one of the shortest known orbital periods among
V523_Cassiopeiae
Variable star in the constellation Corona Australis
apparent magnitudes of 4.74 to 5 over 14 hours, this is the brightest W Ursae Majoris variable (low mass contact binary) in the night sky. Based on parallax measurements
Epsilon_Coronae_Australis
Contact binary star system
Karen (2013-10-01). "To Pulsate or to Eclipse? Status of KIC 9832227 Variable Star". arXiv:1310.0544 [astro-ph.SR]. Molnar, Lawrence A.; Van Noord, Daniel
KIC_9832227
Spectroscopic binary star system in the constellation Ursa Major
c Ursae Majoris is the Bayer designation for a double-lined spectroscopic binary star system in the northern constellation of Ursa Major. It has an apparent
C_Ursae_Majoris
Binary star in the constellation Ursa Major
Tau Ursae Majoris (τ UMa) is the Bayer designation for a binary star in the northern circumpolar constellation of Ursa Major. It is visible to the naked
Tau_Ursae_Majoris
Triple star system in the constellation Boötes
magnitude of +4.83. The companion component, 44 Boötis B, is a W Ursae Majoris variable spectroscopic binary. The variability of this star system was discovered
44_Boötis
Gravitationally-binding region around a star in a binary system
such times, the system manifests as a contact binary such as a W Ursae Majoris variable. AS slow contact Similar to AR, but only a short period of fast
Roche_lobe
Binary star in the constellation Pegasus
relative luminosities and radii. It was determined to be a variable of the W Ursae Majoris type, and in 1945 the orbital period was shown to vary over
U_Pegasi
Class of eclipsing binary stars
This distinguishes them from the so-called beta Lyrae variables and W Ursae Majoris variables, where the two components are so close that gravitational
Algol_variable
Variable star in the constellation Vulpecula
in the northern constellation of Vulpecula, abbreviated ER Vul. It is a variable star system with a brightness that ranges from an apparent visual magnitude
ER_Vulpeculae
Contact binary star system in the constellation Ara
4 cluster. The system ASASSN-V J173229.06−613712.5 belongs to the W Ursae Majoris type of close contact binary systems. Analysis of TESS space telescope
ASASSN-V_J173229.06−613712.5
Star in the constellation Phoenix
temperatures of 6,083 and 6,310 K, the system is classified as a W Ursae Majoris variable of subtype W, where the secondary star is hotter than the primary; for
AE_Phoenicis
Star system in the constellation Cepheus
Sun. The two inner components form an eclipsing contact binary of W Ursae Majoris-type, whose two component stars share a common outer layer. Both are
VW_Cephei
Solitary red giant star in the constellation Ursa Major
Rho Ursae Majoris (ρ UMa) is the Bayer designation for a solitary star in the northern circumpolar constellation of Ursa Major. It is often faintly visible
Rho_Ursae_Majoris
Star in the constellation Virgo
found to be variable by P. Guthnick and R. Prager in 1929, and designated AH Vir. This component was determined to be a W Ursae Majoris variable, and an orbital
AH_Virginis
Type of variable stellar binary
sharply defined). On the other hand, beta Lyrae variables look somewhat like W Ursae Majoris variables; however, the latter are in general yet closer binaries
Beta_Lyrae_variable
Star in the constellation Ursa Minor
more likely derived from Alrucaba or Rucaba, a name applied to Theta Ursae Majoris. In 2016, the International Astronomical Union organized a Working Group
Kochab
Natural physical entity in space
through a region containing an intrinsic variable type, then its physical properties can cause it to become a variable star. An example of this is the instability
Astronomical_object
Star system in the Ursa Major
discovered in the universe. The two inner components form a close W Ursae Majoris-type contact binary system. The primary star has a mass of approximately
TYC_3801-1529-1
Binary system in the constellation Ursa Major
asterism consisting of ω Ursae Majoris, 57 Ursae Majoris, 47 Ursae Majoris, 58 Ursae Majoris, 49 Ursae Majoris and 56 Ursae Majoris. Consequently, the Chinese
Omega_Ursae_Majoris
Star in the constellation Centaurus
Bilir, S; Karatas, Y; Demircan, O; Eker, Z (2005). "Kinematics of W Ursae Majoris type binaries and evidence of the two types of formation". Monthly
RR_Centauri
Binary star in the Andromeda constellation
cycle of roughly 8 hours. The observed variability is typical of W Ursae Majoris variable stars, so the two stars in this system form a contact binary. The
AB_Andromedae
Triple star system
is a shallow contact binary system, belonging to sub-type A of the W Ursae Majoris class. It has an orbital period of 8.1924 hours and a semimajor axis
EQ_Tauri
Binary star system in the constellation Ursa Major
and W = 7. They are members of the halo population of the Milky Way galaxy. The secondary is a flare star that is referred to as WX Ursae Majoris. It
Gliese_412
Eclipsing binary star system in the constellation Andromeda
specify the onset time of the eclipses, it is classified as a W Ursae Majoris variable star. It is also observed as an X-ray source and is a member of
QX_Andromedae
Star system in the constellation Ursa Major
catalogue of infrared objects, and has been given the variable star designation KV Ursae Majoris. Much of what is known about XTE J1118+480 comes from
XTE_J1118+480
Star in the constellation Ursa Minor
understood to be coming from the same object. It is classified as a SU Ursae Majoris variable subclass of dwarf nova in that it has both 'normal' outbursts of
SS_Ursae_Minoris
Constellation in the Southern Celestial Hemisphere
is an eclipsing binary that is also a contact binary known as a W Ursae Majoris variable. The two component stars orbit closely enough to each other for
Corvus_(constellation)
Difference of intensity of the stellar continuum spectrum
Space Telescope Eclipse Observations of the Nova‐like Cataclysmic Variable UX Ursae Majoris". The Astrophysical Journal. 499 (1): 414–428. arXiv:astro-ph/9801206
Balmer_jump
Binary star in the constellation Cepheus
WZ Cephei is an eclipsing binary star of W Ursae Majoris-type in the constellation of Cepheus, located 976 light years away from the Sun. The stars orbit
WZ_Cephei
Star in the constellation Centaurus
temperatures of 5,955 and 6,221 K, the system is classified as a W Ursae Majoris variable of subtype W, where the secondary star is hotter than the primary; for
V752_Centauri
Open cluster in the constellation Puppis
and in a further study one more eclipsing binary (specifically a W Ursae Majoris variable) was found to lie at the background. "NGC 2539". SIMBAD. Centre
NGC_2539
Constellation in the southern celestial hemisphere
TY Mensae is another eclipsing binary system classified as a W Ursae Majoris variable; the two components are so close that they share a common envelope
Mensa_(constellation)
Stars with irregular large fluctuations in brightness
In astronomy, cataclysmic variable stars (CVs) are stars which irregularly increase in brightness by a large factor, then drop back down to a quiescent
Cataclysmic_variable_star
Eclipsing binary star in the constellation Corvus
over 7.6 hours. The system is a contact binary also known as a W Ursae Majoris variable, where the two component stars orbit closely enough to each other
SX_Corvi
Constellation in the Southern Celestial Hemisphere
to 6.83 over a period of 15.6 hours. The system is classed as a W Ursae Majoris variable—the primary is hotter than the secondary and the drop in magnitude
Antlia
Overview of the scientific field of astronomy
Alpha² Canum Venaticorum variable SX Arietis Pulsar Eclipsing binary Algol variable Beta Lyrae variable W Ursae Majoris variable Supernova Classes Type
Outline_of_astronomy
Binary star in the constellation Canis Minor
Roche lobes, becoming a W Ursae Majoris variable (also known as a low mass contact binary). YY CMi was first reported to be variable in August 1934 by Otto
YY_Canis_Minoris
Star in the constellation Ursa Major
include HD 103095, HR 4550, and Gliese 451. It has the variable star designation CF Ursae Majoris, which originally referred to a supposed flaring companion
Groombridge_1830
Star in the constellation Cygnus
the variable star designation for an overcontact binary star system in the constellation Cygnus. First found to be variable in 1965, it is a W Ursae Majoris
V1191_Cygni
Nova that occurred in 2025
days) periods. It is thus classified as a dwarf nova of the SU Ursae Majoris variable type. A spectrum taken of 572 Velorum on 30 June 2025 looks typical
V572_Velorum
Open cluster in the constellation Cygnus
Doradus variables, with four eclipsing binaries, and 106 stars displaying rotational modulation that is indicative of star spots. Two systems are W Ursae Majoris
NGC_6866
Former constellation
tail of Ursa Major, containing stars between β Bootis (Nekkar) and η Ursae Majoris (Alkaid). Johann Elert Bode converted its name to Latin as Quadrans
Quadrans_Muralis
Highly magnetic type of cataclysmic variable binary star system
(1000–8000 teslas). The WD in the polar AN Ursae Majoris has the strongest known magnetic field among cataclysmic variables, with a field strength of 230 million
Polar_(star)
Classification of stars based on spectral properties
standards: F0IIIa – Zeta Leonis F0Ib – Alpha Leporis F1V - 37 Ursae Majoris F2V – 78 Ursae Majoris F7V - Iota Piscium F9V - Beta Virginis F9V - HD 10647 G-type
Stellar_classification
Star in the constellation Hercules
AM Herculis is a binary variable star located in the constellation Hercules. This star, along with the star AN Ursae Majoris, is the prototype for a category
AM_Herculis
Stellar classification
unchanged over years, are Chara (G0V), the Sun (G2V), Kappa1 Ceti (G5V), 61 Ursae Majoris (G8V). Other primary MK standard stars include HD 115043 (G1V) and 16
G-type_main-sequence_star
Open cluster in the constellation Cepheus
appears to be a W Ursae Majoris type. A further study in 2004 identified further 10 variables near the cluster, five of which were W Ursae Majoris type and one
NGC_6939
Star system in the constellation Leo Minor
system was found to be variable using observations with the Hipparcos satellite. It is classified as an A-type W Ursae Majoris eclipsing binary, where
VW_Leonis_Minoris
Open cluster in the constellation Andromeda
straggler star is also present, along with some spectroscopic binaries and variable stars. The detached eclipsing binary DS Andromedae is a member of this
NGC_752
Type of variable star
Mira variables (/ˈmaɪrə/; named for the prototype star Mira) are a class of pulsating stars characterized by very red colours, pulsation periods longer
Mira_variable
Eclipsing binary star in the constellation Virgo
system with an orbital period of 15.4 hours. It is classified as a W Ursae Majoris variable, which means the components are in near contact with each other
AG_Virginis
Star in the constellation Phoenix
light-years (201 parsecs) from Earth. AD Phoenicis is a contact binary of W Ursae Majoris type, composed of two stars so close that their surfaces touch each
AD_Phoenicis
System of two stars orbiting each other
star was computed in 1827, when Félix Savary computed the orbit of Xi Ursae Majoris. Over the years, many more double stars have been catalogued and measured
Binary_star
Variable star in the constellation Pisces
suggested this is a contact binary. It was confirmed as a W Ursae Majoris (W UMa) variable using photometric observations made by J. Moorhead. O. J. Eggen
VZ_Piscium
W URSAE-MAJORIS-VARIABLE
W URSAE-MAJORIS-VARIABLE
W URSAE-MAJORIS-VARIABLE
W URSAE-MAJORIS-VARIABLE
W URSAE-MAJORIS-VARIABLE
W URSAE-MAJORIS-VARIABLE
W URSAE-MAJORIS-VARIABLE
W URSAE-MAJORIS-VARIABLE
W URSAE-MAJORIS-VARIABLE