WASP-48

{{Starbox begin

| name = WASP-48

}}

{{Starbox observe

| constell = Cygnus{{cite constellation|WASP-48}}

| epoch = J2000

| ra = {{RA|19|24|38.9614}}

| dec = {{DEC|+55|28|23.332}}

| appmag_v = 11.65{{±|0.14}}{{cite journal |bibcode=2000A&A...355L..27H |title=The Tycho-2 catalogue of the 2.5 million brightest stars |last1=Høg |first1=E. |last2=Fabricius |first2=C. |last3=Makarov |first3=V. V. |last4=Urban |first4=S. |last5=Corbin |first5=T. |last6=Wycoff |first6=G. |last7=Bastian |first7=U. |last8=Schwekendiek |first8=P. |last9=Wicenec |first9=A. |journal=Astronomy and Astrophysics |date=2000 |volume=355 }}

}}

{{Starbox character

| type = main sequence

| class = G0V{{cite journal |bibcode=2025A&A...694A..91Z |title=Stellar obliquities of eight close-in gas giant exoplanets |last1=Zak |first1=J. |last2=Boffin |first2=H. M. J. |last3=Sedaghati |first3=E. |last4=Bocchieri |first4=A. |last5=Balkoova |first5=Z. |last6=Skarka |first6=M. |last7=Kabath |first7=P. |journal=Astronomy and Astrophysics |date=2025 |volume=694 |pages=A91 |doi=10.1051/0004-6361/202452171 |arxiv=2501.05615 }}

}}

{{Starbox astrometry

| radial_v = {{val|−19.47|0.65}}

| prop_mo_ra = +6.210

| prop_mo_dec = −28.007

| parallax = 2.1639

| p_error = 0.0104

| parallax_footnote = {{cite Gaia DR3|2141754578242371584}}

}}

{{Starbox detail

| source =

| mass = 1.09{{±|0.08}}{{cite journal |bibcode=2025A&A...694A..91Z |title=Stellar obliquities of eight close-in gas giant exoplanets |last1=Zak |first1=J. |last2=Boffin |first2=H. M. J. |last3=Sedaghati |first3=E. |last4=Bocchieri |first4=A. |last5=Balkoova |first5=Z. |last6=Skarka |first6=M. |last7=Kabath |first7=P. |journal=Astronomy and Astrophysics |date=2025 |volume=694 |pages=A91 |doi=10.1051/0004-6361/202452171 |arxiv=2501.05615 }}

| radius = 1.09{{±|0.14}}

| gravity = 4.03{{±|0.03}}{{cite journal|arxiv=1104.2827|title=WASP-35b, WASP-48b and WASP-51b: Two new planets and an independent discovery of HAT-P-30b|year=2011|doi=10.1088/0004-6256/142/3/86|last1=Enoch|first1=B.|last2=Anderson|first2=D. R.|last3=Barros|first3=S. C. C.|last4=Brown|first4=D. J. A.|last5=Collier Cameron|first5=A.|last6=Faedi|first6=F.|last7=Gillon|first7=M.|last8=Hébrard|first8=G.|last9=Lister|first9=T. A.|last10=Queloz|first10=D.|last11=Santerne|first11=A.|last12=Smalley|first12=B.|last13=Street|first13=R. A.|last14=Triaud|first14=A. H. M. J.|last15=West|first15=R. G.|last16=Bouchy|first16=F.|last17=Bento|first17=J.|last18=Butters|first18=O.|last19=Fossati|first19=L.|last20=Haswell|first20=C. A.|last21=Hellier|first21=C.|last22=Holmes|first22=S.|last23=Jehen|first23=E.|last24=Lendl|first24=M.|last25=Maxted|first25=P. F. L.|last26=McCormac|first26=J.|last27=Miller|first27=G. R. M.|last28=Moulds|first28=V.|last29=Moutou|first29=C.|last30=Norton|first30=A. J.|journal=The Astronomical Journal |volume=142 |issue=3 |page=86 |bibcode=2011AJ....142...86E |s2cid=63996398|display-authors=29}}

| luminosity = 3.8{{cite journal |bibcode=2020ApJ...890...23L |title=Current Population Statistics do Not Favor Photoevaporation over Core-powered Mass Loss as the Dominant Cause of the Exoplanet Radius Gap |last1=Loyd |first1=R. O. Parke |last2=Shkolnik |first2=Evgenya L. |last3=Schneider |first3=Adam C. |last4=Richey-Yowell |first4=Tyler |last5=Barman |first5=Travis S. |last6=Peacock |first6=Sarah |last7=Pagano |first7=Isabella |journal=The Astrophysical Journal |date=2020 |volume=890 |issue=1 |page=23 |doi=10.3847/1538-4357/ab6605 |doi-access=free |arxiv=1912.12305 }}

| temperature = 6,000{{±|150}}

| metal = −0.12{{±|0.12}}

| rotation = {{val|7.2|0.5|u= days}}

| rotational_velocity = 12.2{{±|0.7}}

| age_gyr = 7.9{{±|2.0|1.6}}

}}

{{Starbox catalog

| names = {{odlist | TYC=3925-739-1 | GSC=03925-00739 | 2MASS=J19243895+5528233 | TIC=284475976 | TOI=1628 | WASP=48}}

}}

{{Starbox reference

| Simbad = WASP-48

| NSTED = WASP-48

}}

{{Starbox end}}

WASP-48 is a G-type main-sequence star about 1,500 light-years away in the constellation Cygnus. The star is likely older than the Sun and slightly depleted in heavy elements. It shows an infrared excess noise of unknown origin,{{cite journal|arxiv=1202.2799|year=2012|doi=10.1086/665043|last1=Sada|first1=Pedro V.|last2=Deming|first2=Drake|last3=Jennings|first3=Donald E.|last4=Jackson|first4=Brian k.|last5=Hamilton|first5=Catrina M.|last6=Fraine|first6=Jonathan|last7=Peterson|first7=Steven W.|last8=Haase|first8=Flynn|last9=Bays|first9=Kevin|last10=Lunsford|first10=Allen|last11=o'Gorman|first11=Eamon|title=Extrasolar Planet Transits Observed at Kitt Peak National Observatory|s2cid=29665395|journal=Publications of the Astronomical Society of the Pacific|volume=124|issue=913|pages=212–229|bibcode=2012PASP..124..212S}} yet has no detectable ultraviolet emissions associated with starspot activity.{{cite journal|doi=10.1088/0004-637X/766/1/9|title=An Ultraviolet Investigation of Activity on Exoplanet Host Stars|year=2013|last1=Shkolnik|first1=Evgenya L.|s2cid=118415788|journal=The Astrophysical Journal|volume=766|issue=1|page=9|arxiv=1301.6192|bibcode=2013ApJ...766....9S}} The discrepancy may be due to large interstellar absorption of light in interstellar medium for WASP-48.{{cite journal|arxiv=1702.02883|title=The effect of ISM absorption on stellar activity measurements and its relevance for exoplanet studies|year=2017|doi=10.1051/0004-6361/201630339|last1=Fossati|first1=L.|last2=Marcelja|first2=S. E.|last3=Staab|first3=D.|last4=Cubillos|first4=P. E.|last5=France|first5=K.|last6=Haswell|first6=C. A.|last7=Ingrassia|first7=S.|last8=Jenkins|first8=J. S.|last9=Koskinen|first9=T.|last10=Lanza|first10=A. F.|last11=Redfield|first11=S.|last12=Youngblood|first12=A.|last13=Pelzmann|first13=G.|s2cid=17549819|journal=Astronomy & Astrophysics|volume=601|pages=A104|bibcode=2017A&A...601A.104F}} The measurements are compounded by the emission from eclipsing contact binary NSVS-3071474 projected on sky plane nearby,{{cite journal|arxiv=1503.00762|title=Physical properties of the HAT-P-23 and WASP-48 planetary systems from multi-colour photometry|year=2015|doi=10.1051/0004-6361/201425449|last1=Ciceri|first1=S.|last2=Mancini|first2=L.|last3=Southworth|first3=J.|last4=Bruni|first4=I.|last5=Nikolov|first5=N.|last6=d'Ago|first6=G.|last7=Schröder|first7=T.|last8=Bozza|first8=V.|last9=Tregloan-Reed|first9=J.|last10=Henning|first10=Th.|s2cid=53607610|journal=Astronomy & Astrophysics|volume=577|pages=A54|bibcode=2015A&A...577A..54C}} although no true stellar companions were detected by survey in 2015.{{cite journal|arxiv=1507.01938|title=A Lucky Imaging search for stellar companions to transiting planet host stars|year=2015|doi=10.1051/0004-6361/201424091|last1=Wöllert|first1=Maria|last2=Brandner|first2=Wolfgang|last3=Bergfors|first3=Carolina|last4=Henning|first4=Thomas|s2cid=119250579|journal=Astronomy & Astrophysics|volume=575|pages=A23|bibcode=2015A&A...575A..23W}}

The star is rotating rapidly, being spun up by the tides raised by the giant planet on close orbit.{{cite journal|arxiv=1406.4402|title=Discrepancies between isochrone fitting and gyrochronology for exoplanet host stars?|year=2014|doi=10.1093/mnras/stu950|last1=Brown|first1=D. J. A.|s2cid=56052792|journal=Monthly Notices of the Royal Astronomical Society|volume=442|issue=2|pages=1844–1862|doi-access=free |bibcode=2014MNRAS.442.1844B}}