65 Aurigae

{{short description|Binary star system in the constellation Auriga}}

{{Starbox begin}}

{{Starbox observe

| epoch=J2000

| ra={{RA|07|22|02.61744}}

| dec={{DEC|+36|45|38.0957}}

| appmag_v=5.12

| constell=Auriga

}}

{{Starbox character

| class=K0 III

| r-i =

| v-r =

| b-v = {{Val|1.082|0.005}}

| u-b =

| variable=

}}

{{Starbox astrometry

| radial_v={{Val|21.81|0.16}}

| prop_mo_ra=−96.915

| prop_mo_dec=−22.436

| parallax=12.9673

| p_error=0.1294

| parallax_footnote =

| absmag_v=0.82

}}

{{Starbox detail

| component1=65 Aur A

| mass=1.34

| radius={{Val|13.02|0.47|2.57}}

| luminosity={{Val|69.6|0.9}}

| temperature={{Val|4575|17|fmt=commas}}

| metal_fe={{Val|−0.35|0.04}}

| gravity=2.72

| rotational_velocity=0.0

| age_gyr=3.31

}}

{{Starbox catalog |

names={{odlist | F=65 Aur | BD=+37°1707 | FK5=2568 | HD=57264 | HIP=35710 | HR=2793 | SAO=60010 }}

}}

{{Starbox reference

| Simbad=65+Aur

}}

{{Starbox end}}

65 Aurigae is a binary star system located 252 light years away from the Sun in the northern constellation of Auriga. It is visible to the naked eye as a faint, orange hued star with an apparent visual magnitude of 5.12. The primary, designated component A, is an aging giant star with a stellar classification of K0 III. It is 3.31 billion years old and has expanded to 13 times the Sun's radius after exhausting the hydrogen at its core. Its companion, component B, is a magnitude 11.7 star located at an angular separation of {{Val|11.4|ul=arcsecond}} from the primary, as of 2008. The pair are moving further from the Earth with a heliocentric radial velocity of 22 km/s.

It was also known to be part of a much bigger constellation named Telescopium Herschelii before it was unrecognized by the International Astronomical Union (IAU).

References

{{Reflist|refs=

{{cite DR2|898059352148520960}}

{{cite simbad | title=65 Aur | access-date=2019-05-25 }}

{{citation

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{{citation

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}}

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| journal=The Astronomical Journal | postscript=.

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{{citation

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| journal=Monthly Notices of the Royal Astronomical Society

| volume=389 | issue=2 | pages=869–879 | date=September 2008

| doi=10.1111/j.1365-2966.2008.13596.x | doi-access=free | postscript=.

| bibcode=2008MNRAS.389..869E | arxiv=0806.2878 | s2cid=14878976 }}

}}