<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
<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
which is bigger vy canis majoris vs uy scuti
which is bigger vy canis majoris vs uy scuti
UY Scuti
UY Scuti