<Li> A survey of the Magellanic Clouds have catalogued many red supergiants, where more than 50 of them exceed 700 R (490,000,000 km; 3.3 AU; 300,000,000 mi). Largest of these is about 1,200--1,300 R . </Li> <Li> Another survey of the star cluster Westerlund 1 revealed that there are several red supergiants or red hypergiants that probably exceed 2,000 R. Westerlund 1 - 26 is in this list . </Li> <Table> List of the largest stars <Tr> <Th> Star name </Th> <Th> Solar radii (Sun = 1) </Th> <Th> Notes </Th> </Tr> <Tr> <Td> Orbit of Saturn </Td> <Td> 1,940--2,169 </Td> <Td> Reported for reference </Td> </Tr> <Tr> <Td> UY Scuti </Td> <Td> 1,708 ± 192 </Td> <Td> Margin of error in size determination: ± 192 solar radii . At the smallest, it would have a size similar to VX Sagittarii (see below) </Td> </Tr> <Tr> <Td> WOH G64 </Td> <Td> 1,540 ± 77 </Td> <Td> This would be the largest star in the LMC, but is unusual in position and motion and might still be a foreground halo giant . Ohnaka (2009) calculates 1,730 R . </Td> </Tr> <Tr> <Td> RW Cephei </Td> <Td> 1,535 </Td> <Td> RW Cep is variable both in brightness (by at least a factor of 3) and spectral type (observed from G8 to M), thus probably also in diameter . Because the spectral type and temperature at maximum luminosity are not known, the quoted sizes are just estimates . </Td> </Tr> <Tr> <Td> Westerlund 1 - 26 </Td> <Td> 1,530 - 1,580 (--2,000) </Td> <Td> Very uncertain parameters for an unusual star with strong radio emission . The spectrum is variable but apparently the luminosity is not . </Td> </Tr> <Tr> <Td> VX Sagittarii </Td> <Td> 1,520 </Td> <Td> VX Sgr is a pulsating variable with a large visual range from 1,350 R to 1,940 R and varies significantly in size . </Td> </Tr> <Tr> <Td> HR 5171 A </Td> <Td> 1,490 ± 540 </Td> <Td> HR 5171 A is a highly distorted star in a close binary system, losing mass to the secondary . Traditionally, it is considered a particularly large yellow hypergiant, although the latest research suggests it is a red supergiant . The variation in temperature is not clear because the size also varies from 1,315 ± 260 R to 1,575 ± 400 R . </Td> </Tr> <Tr> <Td> KY Cygni </Td> <Td> 1,420--2,850 </Td> <Td> The upper estimate is due to an unusual K band measurement and thought to be an artifact of a reddening correction error, and is thought to be against stellar evolutionary theory . The lower estimate is consistent with other stars in the same survey and with theoretical models . </Td> </Tr> <Tr> <Td> VY Canis Majoris </Td> <Td> 1,420 ± 120 </Td> <Td> Once thought to be a star so large that it contradicted stellar evolutionary theory with a radius of 1,800 R to 2,200 R, improved measurements have brought it down to size . </Td> </Tr> <Tr> <Td> AH Scorpii </Td> <Td> 1,411 ± 124 </Td> <Td> AH Sco is variable by nearly 3 magnitudes in the visual range, and an estimated 20% in total luminosity . The variation in diameter is not clear because the temperature also varies . </Td> </Tr> <Tr> <Td> VV Cephei A </Td> <Td> 1,400 or 1,050--1,800 </Td> <Td> VV Cep A is a highly distorted star in a close binary system, losing mass to the secondary for at least part of its orbit . Older estimates have given much larger sizes . </Td> </Tr> <Tr> <Td> IRC + 10420 (V1302 Aquilae) </Td> <Td> 1,342 </Td> </Tr> <Tr> <Td> SMC 018136 </Td> <Td> 1,310 </Td> <Td> This would be the largest star in the SMC . </Td> </Tr> <Tr> <Td> Mu Cephei (Herschel's "Garnet Star") </Td> <Td> 1,260 </Td> <Td> Other recent estimates range from 650 R to 1,420 R </Td> </Tr> <Tr> <Td> BI Cygni </Td> <Td> 1,240 </Td> </Tr> <Tr> <Td> S Persei </Td> <Td> 1,212 ± 124 </Td> <Td> In the Perseus Double Cluster . Other recent estimates range from 780 R to 1,230 R . </Td> </Tr> <Tr> <Td> RAFGL 2139 </Td> <Td> 1,200 </Td> <Td> RAFGL 2139 is a rare red supergiant companion to WR 114 that has a bow shock . </Td> </Tr> <Tr> <Td> PZ Cassiopeiae </Td> <Td> 1,190 - 1,940 or 1,260 - 1,340 </Td> <Td> The largest estimate is due to an unusual K band measurement and thought to be an artifact of a reddening correction error . The lowest estimate is consistent with other stars in the same survey and with theoretical models, and the intermediate ones have been obtained refining the distance to this star, and thus its parameters . </Td> </Tr> <Tr> <Td> NML Cygni </Td> <Td> 1,183--2,770 </Td> <Td> An accurate measure of its distance and its luminosity combined with assumptions of its temperature give 1,640 R for 3,250 K or 2,770 R for 2,500 K . </Td> </Tr> <Tr> <Td> EV Carinae </Td> <Td> 1,168 - 2,880 </Td> <Td> EV Car is an unstable star plagued by dust extinction . The value on the left is subject to inaccuracy and thus not yet well defined . </Td> </Tr> <Tr> <Td> BC Cygni </Td> <Td> 1,140 - 1,230 </Td> <Td> Other recent estimates range from 856 R to 1,553 R . </Td> </Tr> <Tr> <Td> RT Carinae </Td> <Td> 1,090 </Td> </Tr> <Tr> <Td> V396 Centauri </Td> <Td> 1,070 </Td> </Tr> <Tr> <Td> Orbit of Jupiter </Td> <Td> 1,064--1,173 </Td> <Td> Reported for reference </Td> </Tr> <Tr> <Td> HV 11423 </Td> <Td> 1,060--1,220 </Td> <Td> HV 11423 is variable in spectral type (observed from K0 to M5), thus probably also in diameter . In October 1978, it was a star of M0I type . </Td> </Tr> <Tr> <Td> CK Carinae </Td> <Td> 1,060 </Td> </Tr> <Tr> <Td> U Lacertae </Td> <Td> 1,025 </Td> </Tr> <Tr> <Td> KW Sagittarii </Td> <Td> 1,009 - 1,460 </Td> <Td> Margin of possible error: ± 142 solar radii (Torres 2013). </Td> </Tr> <Tr> <Td> NR Vulpeculae </Td> <Td> 980 </Td> </Tr> <Tr> <Td> GCIRS 7 </Td> <Td> 960 ± 92 </Td> </Tr> <Tr> <Td> S Cassiopeiae </Td> <Td> 930 </Td> </Tr> <Tr> <Td> IX Carinae </Td> <Td> 920 </Td> </Tr> <Tr> <Td> HV 2112 </Td> <Td> 918 </Td> <Td> Most likely candidate for a Thorne - Zytkow Object . </Td> </Tr> <Tr> <Td> NSV 25875 </Td> <Td> 891 </Td> </Tr> <Tr> <Td> Betelgeuse (Alpha Orionis) </Td> <Td> 887--955 </Td> <Td> Margin of possible error: ± 203 solar radii (Dolan 2016) or ± 217 solar radii (Neilson 2011). At the largest, it would have a size similar to Jupiter's orbit </Td> </Tr> <Tr> <Td> V437 Scuti </Td> <Td> 874 </Td> </Tr> <Tr> <Td> V602 Carinae </Td> <Td> 860 - 1,050 </Td> <Td> Margin of possible error: ± 165 solar radii (Torres 2015). </Td> </Tr> <Tr> <Td> V669 Cassiopeiae </Td> <Td> 859 </Td> </Tr> <Tr> <Td> V1185 Scorpii </Td> <Td> 830 </Td> </Tr> <Tr> <Td> Outer limits of the asteroid belt </Td> <Td> 816 </Td> <Td> Reported for reference </Td> </Tr> <Tr> <Td> BO Carinae </Td> <Td> 790 </Td> </Tr> <Tr> <Td> SU Persei </Td> <Td> 780 </Td> <Td> In the Perseus Double Cluster </Td> </Tr> <Tr> <Td> RS Persei </Td> <Td> 770 - 1,000 </Td> <Td> In the Perseus Double Cluster . Margin of possible error: ± 30 solar radii (Baron 2014). </Td> </Tr> <Tr> <Td> AV Persei </Td> <Td> 770 </Td> <Td> In the Perseus Double Cluster </Td> </Tr> <Tr> <Td> V355 Cepheus </Td> <Td> 300 - 770 </Td> </Tr> <Tr> <Td> V915 Scorpii </Td> <Td> 760 </Td> </Tr> <Tr> <Td> S Cephei </Td> <Td> 760 </Td> </Tr> <Tr> <Td> HD 303250 </Td> <Td> 750 </Td> </Tr> <Tr> <Td> V382 Carinae </Td> <Td> 747 </Td> <Td> The brightest yellow hypergiant in the night sky, one of the rarest types of star . Achmad (1992) calculates 600 R to 1,100 R or 700 ± 250 R . </Td> </Tr> <Tr> <Td> RU Virginis </Td> <Td> 742 </Td> </Tr> <Tr> <Td> V648 Cassiopeiae </Td> <Td> 710 </Td> </Tr> <Tr> <Td> XX Persei </Td> <Td> 710 </Td> <Td> In the Perseus Double Cluster </Td> </Tr> <Tr> <Td> TV Geminorum </Td> <Td> 620 - 710 (--770) </Td> </Tr> <Tr> <Td> HD 179821 </Td> <Td> 704 </Td> <Td> This star is a yellow hypergiant although most authors consider it as a supergiant, a protoplanetary nebula or a post-AGB star </Td> </Tr> <Tr> <Td> V528 Carinae </Td> <Td> 700 </Td> </Tr> <Tr> <Th_colspan="5"> The following well - known stars are listed for the purpose of comparison . </Th> </Tr> <Tr> <Td> V354 Cephei </Td> <Td> 690 - 1,520 </Td> </Tr> <Tr> <Td> Antares A (Alpha Scorpii A) </Td> <Td> 680 </Td> <Td> Other recent estimates range from 653 R to 1,246 R . </Td> </Tr> <Tr> <Td> CE Tauri </Td> <Td> 608 </Td> <Td> Can be occulted by the Moon, allowing accurate determination of its apparent diameter . </Td> </Tr> <Tr> <Td> R Leporis (Hind's "Crimson Star") </Td> <Td> 400--535 </Td> <Td> Margin of possible error: ± 90 solar radii . </Td> </Tr> <Tr> <Td> Rho Cassiopeiae </Td> <Td> 400 - 500 </Td> <Td> Yellow hypergiant, one of the rarest types of a star . </Td> </Tr> <Tr> <Td> Inner limits of the asteroid belt </Td> <Td> 412 </Td> <Td> Reported for reference </Td> </Tr> <Tr> <Td> Mira A (Omicron Ceti) </Td> <Td> 332--402 </Td> <Td> Prototype Mira variable . De beck (2005) calculates 541 R . </Td> </Tr> <Tr> <Td> V509 Cassiopeiae </Td> <Td> 400--900 </Td> <Td> Yellow hypergiant, one of the rarest types of a star . </Td> </Tr> <Tr> <Td> CW Leonis </Td> <Td> 390--500 </Td> <Td> CW Leonis has been one of the mistaken identities as the claimed planet "Nibiru" or "Planet X", due to its brightness as it approaches 1st magnitude . Other recent estimates range from 700 R to 826 R . </Td> </Tr> <Tr> <Td> V838 Monocerotis </Td> <Td> 380 (in 2009) </Td> <Td> A short time after the outburst V838 Mon was measured at 1,570 ± 400 R. However the distance to this "L supergiant", and hence its size, have since been reduced and it proved to be a transient object that shrunk about four-fold over a few years . </Td> </Tr> <Tr> <Td> S Doradus </Td> <Td> 100 - 380 </Td> <Td> Prototype S Doradus variable </Td> </Tr> <Tr> <Td> R Doradus </Td> <Td> 370 </Td> <Td> Star with the second largest apparent size after the Sun . </Td> </Tr> <Tr> <Td> The Pistol Star </Td> <Td> 340 </Td> <Td> Blue hypergiant, among the most massive and luminous stars known . </Td> </Tr> <Tr> <Td> La Superba (Y Canum Venaticorum) </Td> <Td> 307 - 390 </Td> <Td> Currently one of the coolest and reddest stars . </Td> </Tr> <Tr> <Td> Orbit of Mars </Td> <Td> 297--358 </Td> <Td> Reported for reference </Td> </Tr> <Tr> <Td> Alpha Herculis (Ras Algethi) </Td> <Td> 284 ± 60 </Td> <Td> Moravveji et al also gives a range from 264 R to 303 R. At an estimated distance of 110 parsecs from the Sun, this corresponds to a radius of 400 ± 61 R . </Td> </Tr> <Tr> <Td> Sun's red giant phase </Td> <Td> 256 349--448 </Td> <Td> The core hydrogen would be exhausted in 5.4 billion years . In 7.647 billion years, The Sun would reach the tip of the red - giant branch of the Hertzsprung--Russell diagram . (see below) Reported for reference </Td> </Tr> <Tr> <Td> Eta Carinae A (Tseen She) </Td> <Td> 250 </Td> <Td> Previously thought to be the most massive single star, but in 2005 it was realized to be a binary system . Its size is poorly defined . one study calculated 60 R, but at optical depth 0.67, the size would be 800 R. At the peak of the Great Eruption, it would have a size similar to VV Cephei A. Other recent estimates range from 85 R to 195 R . </Td> </Tr> <Tr> <Td> Orbit of Earth </Td> <Td> 211--219 </Td> <Td> Reported for reference </Td> </Tr> <Tr> <Td> Deneb (Alpha Cygni) </Td> <Td> 203 </Td> </Tr> <Tr> <Td> LBV 1806 - 20 </Td> <Td> 200 </Td> <Td> Formerly a candidate for the most luminous star in the Milky Way . </Td> </Tr> <Tr> <Td> Orbit of Venus </Td> <Td> 154--157 </Td> <Td> Reported for reference </Td> </Tr> <Tr> <Td> Epsilon Aurigae A (Almaaz) </Td> <Td> 143 - 358 </Td> <Td> ε Aur was incorrectly hailed as the largest star with a radius 2,000 R or 3,000 R, even though it later turned out not to be an infrared light star but rather a dusk torus surrounding the system . </Td> </Tr> <Tr> <Td> Peony Nebula Star </Td> <Td> 100 </Td> <Td> Candidate for most luminous star in the Milky Way . </Td> </Tr> <Tr> <Td> Rigel A (Beta Orionis A) </Td> <Td> 78.9 </Td> </Tr> <Tr> <Td> Canopus (Alpha Carinae) </Td> <Td> 71 </Td> <Td> Second brightest star in the night sky . </Td> </Tr> <Tr> <Td> Orbit of Mercury </Td> <Td> 66--100 </Td> <Td> Reported for reference </Td> </Tr> <Tr> <Td> Aldebaran (Alpha Tauri) </Td> <Td> 44.2 </Td> </Tr> <Tr> <Td> Polaris (Alpha Ursae Minoris) </Td> <Td> 37.5 </Td> <Td> The current northern pole star . </Td> </Tr> <Tr> <Td> R136a1 </Td> <Td> 35.4 </Td> <Td> Also on record as the most massive and luminous star known . </Td> </Tr> <Tr> <Td> Arcturus (Alpha Boötis) </Td> <Td> 25.4 </Td> <Td> Brightest star in the northern hemisphere . </Td> </Tr> <Tr> <Td> HDE 226868 </Td> <Td> 20 - 22 </Td> <Td> The supergiant companion of black hole Cygnus X-1 . The black hole is 500,000 times smaller than the star . </Td> </Tr> <Tr> <Td> VV Cephei B </Td> <Td> 13 - 25 </Td> <Td> The B - type main sequence companion of VV Cephei A . </Td> </Tr> <Tr> <Td> Sun's helium burning phase </Td> <Td> 10 </Td> <Td> After the red - giant branch the Sun has approximately 120 million years of active life left . Reported for reference </Td> </Tr> <Tr> <Td> Sun </Td> <Td> </Td> <Td> The largest object in the Solar System . Reported for reference </Td> </Tr> </Table> <Tr> <Th> Star name </Th> <Th> Solar radii (Sun = 1) </Th> <Th> Notes </Th> </Tr>

Which is bigger vy canis majoris vs uy scuti