BD+48 740#Planetary system

{{Short description|Giant star in the constellation Perseus}}

{{Starbox begin

| name=BD+48 740

}}

{{Starbox observe

| epoch=J2000

| ra={{RA|02|42|58.21780}}{{cite journal|title=Validation of the new Hipparcos reduction|url=http://www.aanda.org/index.php?option=com_article&access=bibcode&Itemid=129&bibcode=2007A%2526A...474..653VFUL|author=van Leeuwen, F. |journal=Astronomy and Astrophysics|volume=474|issue=2|pages=653–664|date=2007|arxiv=0708.1752|bibcode=2007A&A...474..653V|doi=10.1051/0004-6361:20078357|s2cid = 18759600}}

| dec={{DEC|+48|55|48.2155}}

| constell=Perseus

}}

{{Starbox character

| class= K3III{{cite simbad|title=BD+48 740|access-date=7 June 2017}}

}}

{{Starbox astrometry

| radial_v=-5.60 ± 0.51{{cite journal|bibcode=2005A&A...430..165F |title=Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters |journal=Astronomy and Astrophysics |volume=430 |pages=165 |last1=Famaey |first1=B. |last2=Jorissen |first2=A. |last3=Luri |first3=X. |last4=Mayor |first4=M. |last5=Udry |first5=S. |last6=Dejonghe |first6=H. |last7=Turon |first7=C. |year=2005 |doi=10.1051/0004-6361:20041272 |arxiv = astro-ph/0409579 |s2cid=17804304 }}

| prop_mo_ra=-5.94

| prop_mo_dec=-2.02

| parallax=1.36

| p_error=1.13

| parallax_footnote=

}}

{{Starbox detail

| source =

| mass = 1.09{{±|0.16}}

| radius = 10.33{{±|1.81}}

| luminosity = 43.7

| gravity = 2.48{{±|0.04}}

| temperature = 4534{{±|8}}

| metal =

| metal_fe = -0.13{{±|0.06}}

| rotation =

| rotational_velocity = <2.9

| age =

| age_myr =

| age_gyr =

}}

{{Starbox catalog

| names=BD+48 740, AG+48 308, GSC 03304-00090, HIC 12684, HIP 12684, 2MASS J02425822+4855483, PPM 45405, SAO 38272, TYC 3304-90-1

}}

{{Starbox reference

| Simbad=BD%2B48+740}}

{{Starbox end}}

BD+48 740 is a giant star suspected of having recently engulfed one of its planets. The star's atmosphere has an overabundance of lithium, a metal that is destroyed by nuclear reactions in stars.

Planetary system

Detection of variations in the star's radial velocity led to the discovery of the superjovian planet BD+48 740 b in 2012, with the discovery having been confirmed in 2018.{{citation|arxiv=1801.04379|year=2018|title=Tracking Advanced Planetary Systems (TAPAS) with HARPS-N|doi=10.1051/0004-6361/201732161|last1=Adamów|first1=M.|last2=Niedzielski|first2=A.|last3=Kowalik|first3=K.|last4=Villaver|first4=E.|last5=Wolszczan|first5=A.|last6=MacIejewski|first6=G.|last7=Gromadzki|first7=M.|journal=Astronomy & Astrophysics|volume=613|pages=A47|s2cid=56091464}} The planet BD+48 740 b has a minimal mass of 1.7{{Jupiter_mass}} and is in a highly eccentric orbit (its distance from the star ranges from 0.3 to 3 astronomical units), which would destabilize the orbits of any other planets. These indications led the discoverers to the conclusion that another planet has recently plunged into the star, been destroyed, and contributed its lithium content to the star.{{cite journal |bibcode=2012ApJ...754L..15A |title=BD+48 740—Li Overabundant Giant Star with a Planet: A Case of Recent Engulfment? |last1=Adamów |first1=M. |last2=Niedzielski |first2=A. |last3=Villaver |first3=E. |last4=Nowak |first4=G. |last5=Wolszczan |first5=A. |journal=The Astrophysical Journal |year=2012 |volume=754 |issue=1 |pages=L15 |doi=10.1088/2041-8205/754/1/L15 |arxiv=1206.4938 |s2cid=53550985 }}

{{Orbitbox planet begin|name=BD+48 740|semimajor_ref=|period_unit=day

|table_ref=

}}

{{Orbitbox planet

|exoplanet=b

| mass = >1.7{{±|0.7}}

| radius =

| semimajor = 1.7{{±|0.1}}

| period = 733{{±|5|8}}

| eccentricity = 0.76{{±|0.05|0.09}}

| inclination =

}}{{Orbitbox end}}

References

{{reflist}}