U Andromedae

{{Short description|Star in the constellation Andromeda}}

{{distinguish|Upsilon Andromedae{{!}}υ (Upsilon) Andromedae}}

{{Starbox begin

| name= U Andromedae }}

{{Starbox image

| image = 250px

| caption = The visual band light curve of U Andromedae, from AAVSO data

}}

{{Starbox observe

| epoch=J2000

| ra={{RA|01|15|29.69623}}{{cite DR2}}

| dec={{DEC|+40|43|08.3932}}

| appmag_v= 9.0 to 15.0

| constell=Andromeda

}}

{{Starbox character

| class=M6e

| b-v=

| u-b=

| variable=Mira

}}

{{Starbox astrometry

| radial_v= {{val|-4.0|5}}

| prop_mo_ra={{val|11.416|0.321}}

| prop_mo_dec={{val|-8.392|0.297}}

| parallax= 1.4745

| p_error= 0.1511

| parallax_footnote =

| absmag_v=

}}

{{Starbox detail

| mass =

| temperature = 3,288

}}

{{Starbox catalog

| names=HD 7482, BD+39°291a, 2MASS J01152971+4043082, IRAS 01126+4027{{cite simbad | title=U And | access-date=October 8, 2018 }}

}}

{{Starbox reference |

Simbad=U+And

}}

{{Starbox end}}

U Andromedae is a variable star in the constellation of Andromeda, at a distance of approximately {{val|2,200|ul=ly|fmt=commas}}. It is a star of spectral type M6e and it is classified as a Mira variable.

U Andromedae is the variable star designation of this star. Its brightness varies by several magnitudes with a mean period of {{val|347.7|ul=d}}, although the exact length of each cycle is somewhat variable. Similarly, the magnitude of each maximum and minimum varies. The mean apparent magnitude is 11.6, with a mean maximum magnitude of 9.9. The brightest recorded maxima are at magnitude 9.0, and the faintest minima at magnitude 15.0. The rise to maximum brightness is faster than the fall to minimum, taking on average 40% of the period.

The large amplitude, long period, and shape of the light curve mean that U Andromedae is classified as a Mira variable, a type of pulsating asymptotic giant branch (AGB) star. It was first observed to be variable by Thomas D. Anderson during 1894 and 1895. AGB stars have exhausted both hydrogen and helium in their cores and are not massive enough to fuse carbon and oxygen, so they erratically fuse helium and hydrogen shells outside the core.