HAT-P-28#Planetary system

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

{{Starbox begin

| name = HAT-P-28

}}

{{Starbox observe

| constell = Andromeda{{cite constellation|HAT-P-28}}

| epoch = J2000

| ra = {{RA|00|52|00.1876}}

| dec = {{DEC|+34|43|42.205}}

| appmag_v = 13.03

}}

{{Starbox character

| type=main sequence

| class = G3

}}

{{Starbox astrometry

| radial_v = 48.06

| prop_mo_ra = {{val|25.615|(14)}}

| prop_mo_dec = {{val|2.712|(11)}}

| pm_footnote =

| parallax = 2.4728

| p_error = 0.0156

| parallax_footnote =

}}

{{Starbox orbit

| reference =

| primary = HAT-P-28

| name = HAT-P-28 B

| period =

| period_unitless =

| axis = 0.994{{±|0.002}}

| axis_unitless = 404 AU

| eccentricity =

| inclination =

| node =

| periastron =

| periarg =

| periarg_primary =

| k1 =

| k2 =

}}

{{Starbox detail

| source = {{citation|arxiv=1802.05269|year=2018|doi=10.3847/1538-3881/aaaf71|last1=Penev|first1=Kaloyan|last2=Bouma|first2=L. G.|last3=Winn|first3=Joshua N.|last4=Hartman|first4=Joel D.|title=Empirical Tidal Dissipation in Exoplanet Hosts from Tidal Spin-up|journal=The Astronomical Journal|volume=155|issue=4|page=165|pmid=31080254|pmc=6510550|bibcode=2018AJ....155..165P|s2cid=64370118 |doi-access=free }}

| mass = 1.02{{±|0.05}}

| radius = 1.10{{±|0.09|0.07}}

| gravity = 4.36{{±|0.06}}

| luminosity = 1.13{{±|0.23|0.16}}

| temperature = 5680{{±|90}}

| metal_fe = 0.12{{±|0.08}}

| rotation =

| rotational_velocity =0.2{{±|0.5|0.2}}

| age_gyr = 6.1{{±|2.6|1.9}}

}}

{{Starbox catalog

| names = {{odlist|GSC=02284-00503|2MASS=J00520018+3443422|Gaia DR2=363702817083391232}}

}}

{{Starbox reference

| Simbad = HAT-P-28

}}

{{Starbox end}}

HAT-P-28 is the primary of a binary star system about 1320 light-years away. It is a G-type main-sequence star. The star's age is older than the Sun's at 6.1{{±|2.6|1.9}} billion years. HAT-P-28 is slightly enriched in heavy elements, having a 130% concentration of iron compared to the Sun. Evolutionary modelling shows it to be right at the end of its main sequence life. The binary star system is suspected to be surrounded by a debris disk with a 6.1″(2500 AU) radius.{{citation|arxiv=1409.0572|title=Herschel/PACS photometry of transiting-planet host stars with candidate warm debris disks|year=2014|doi=10.1051/0004-6361/201322956|last1=Merín|first1=Bruno|last2=Ardila|first2=David R.|last3=Ribas|first3=Álvaro|last4=Bouy|first4=Hervé|last5=Bryden|first5=Geoffrey|last6=Stapelfeldt|first6=Karl|last7=Padgett|first7=Deborah|journal=Astronomy & Astrophysics|volume=569|pages=A89|bibcode=2014A&A...569A..89M|s2cid=10038821}}

The red dwarf stellar companion was detected in 2015 at a projected separation of 0.972″{{citation|arxiv=1506.05456|title=A Lucky Imaging search for stellar sources near 74 transit hosts|year=2015|doi=10.1051/0004-6361/201526525|last1=Wöllert|first1=Maria|last2=Brandner|first2=Wolfgang|journal=Astronomy & Astrophysics|volume=579|pages=A129|bibcode=2015A&A...579A.129W|s2cid=118903879}} and confirmed in 2016 to be either bound or co-moving.{{citation|arxiv=1606.07102|year=2016|doi=10.3847/0004-637X/827/1/8|last1=Ngo|first1=Henry|last2=Knutson|first2=Heather A.|last3=Hinkley|first3=Sasha|last4=Bryan|first4=Marta|last5=Crepp|first5=Justin R.|last6=Batygin|first6=Konstantin|last7=Crossfield|first7=Ian|last8=Hansen|first8=Brad|last9=Howard|first9=Andrew W.|last10=Johnson|first10=John A.|last11=Mawet|first11=Dimitri|last12=Morton|first12=Timothy D.|last13=Muirhead|first13=Philip S.|last14=Wang|first14=Ji|title=FRIENDS OF HOT JUPITERS. IV. STELLAR COMPANIONS BEYOND 50 au MIGHT FACILITATE GIANT PLANET FORMATION, BUT MOST ARE UNLIKELY TO CAUSE KOZAI–LIDOV MIGRATION|journal=The Astrophysical Journal|volume=827|issue=1|page=8|bibcode=2016ApJ...827....8N|s2cid=41083068 |doi-access=free }}