HD 113337#Planetary system

{{Short description|Binary star system in the constellation Draco}}

{{Starbox begin

| name = HD 113337

}}

{{Starbox observe

| constell = Draco

| epoch = J2000

| ra = {{RA|13|01|46.9269}}

| dec = {{DEC|63|36|36.796}}

| appmag_v = 6.03[http://www.allplanets.ru/star.php?star=HD%20113337 ПЛАНЕТНЫЕ СИСТЕМЫ HD 113337 HIP 63584 HR 4934]

}}

{{Starbox character

| class = F6V+M3.5V+M3.5V

| variable =

}}

{{Starbox astrometry

| component1 = A

| radial_v = {{val|-14.93|0.13}}

| prop_mo_ra = {{val|-173.342|0.035}}

| prop_mo_dec = {{val|24.850|0.027}}

| pm_footnote =

| parallax = 27.6253

| p_error = 0.0253

| parallax_footnote =

| absmag_v = +3.18

}}

{{Starbox orbit

| reference =

| primary = HD 113337

| name =LSPM J1301+6337

| period =

| period_unitless =

| axis = 119″ (4310 AU)

| axis_unitless =

| eccentricity =

| inclination =

| node =

| periastron =

| periarg =

| periarg_primary =

| k1 =

| k2 =

}}

{{Starbox detail

| source ={{citation|arxiv=1905.11156|title=Constraints on HD 113337 fundamental parameters and planetary system. Combining long-base visible interferometry, disc imaging, and high-contrast imaging|year=2020|doi=10.1051/0004-6361/201935494|last1=Borgniet |first1=Simon |last2=Perraut |first2=K. |last3=Su |first3=K. |last4=Bonnefoy |first4=M. |last5=Delorme |first5=Philippe |last6=Lagrange |first6=Anne-Marie |last7=Bailey |first7=V. |last8=Buenzli |first8=E. |last9=Defrère |first9=D. |last10=Henning |first10=T. |last11=Hinz |first11=P. |last12=Leisenring |first12=J. |last13=Meunier |first13=Nadège |last14=Mourard |first14=D. |last15=Nardetto |first15=N. |last16=Skemer |first16=A. |journal=Astronomy & Astrophysics |volume=A44 |page=627 |s2cid=166228639 }}

|component1=HD 113337

|component2=LSPM J1301+6337

| mass = 1.48{{±|0.08}}

| mass2= 0.245*2

| radius = 1.50{{±|0.04}}

| gravity = 4.21{{±|0.08}}

| luminosity = 4.29{{±|0.25}}

| temperature = 6774{{±|125}}

| metal = 0.07{{±|0.02}}

| rotation =

| rotational_velocity = 1.82{{±|0.07}}{{citation |arxiv=1810.08108 |title=SWEET-Cat updated New homogenous spectroscopic parameters |year=2018 |doi=10.1051/0004-6361/201833350 |last1=Sousa |first1=S. G. |last2=Adibekyan |first2=V. |last3=Delgado-Mena |first3=E. |last4=Santos |first4=Nuno C. |last5=Andreasen |first5=D. T. |last6=Ferreira |first6=A. C. S. |last7=Tsantaki |first7=M. |last8=Barros |first8=S. C. C. |last9=Demangeon |first9=O. |last10=Israelian |first10=G. |last11=Faria |first11=J. P. |last12=Figueira |first12=P. |last13=Mortier |first13=A. |last14=Brandao |first14=I. |last15=Montalto |first15=M. |last16=Rojas-Ayala |first16=B. |last17=Santerne |first17=Alexandre |journal=Astronomy & Astrophysics |volume=A58 |page=620 |bibcode=2018A&A...620A..58S |s2cid=119374557 }}

| age_myr = 15{{±|6|1}}

}}

{{Starbox catalog

| names = {{odlist|HD=113337|BD=+64 927|2MASS=J13014695+6336368|Gaia DR2=1676282377934772608|HIP=63584|HR=4934|TYC=4166-541-1}}

}}

{{Starbox reference

| Simbad = HD+113337

}}

{{Starbox end}}

HD 113337 (LDS 2662 A) is the primary component of binary star system LDS 2662, about {{val|118|fmt=commas|u=light-years}} away from Earth. The primary main-sequence star belongs to the spectral class of F6. The star system is extremely young, and it is slightly enriched in heavy elements, with an abundance of such elements at about 115% that of the Sun.

The primary star is surrounded by a debris disk discovered by the Herschel Space Observatory,{{citation|arxiv=1706.01218|title=SONS: The JCMT legacy survey of debris discs in the submillimetre|year=2017|doi=10.1093/mnras/stx1378|last1=Holland|first1=Wayne S.|last2=Matthews|first2=Brenda C.|last3=Kennedy|first3=Grant M.|last4=Greaves|first4=Jane S.|last5=Wyatt|first5=Mark C.|last6=Booth|first6=Mark|last7=Bastien|first7=Pierre|last8=Bryden|first8=Geoff|last9=Butner|first9=Harold|last10=Chen|first10=Christine H.|last11=Chrysostomou|first11=Antonio|last12=Davies|first12=Claire L.|last13=Dent|first13=William R. F.|last14=Di Francesco|first14=James|last15=Duchêne|first15=Gaspard|last16=Gibb|first16=Andy G.|last17=Friberg|first17=Per|last18=Ivison|first18=Rob J.|last19=Jenness|first19=Tim|last20=Kavelaars|first20=JJ|last21=Lawler|first21=Samantha|last22=Lestrade|first22=Jean-François|last23=Marshall|first23=Jonathan P.|last24=Moro-Martin|first24=Amaya|last25=Panić|first25=Olja|last26=Phillips|first26=Neil|last27=Serjeant|first27=Stephen|last28=Schieven|first28=Gerald H.|last29=Sibthorpe|first29=Bruce|last30=Vican|first30=Laura|journal=Monthly Notices of the Royal Astronomical Society|volume=470|issue=3|pages=3606–3663|doi-access=free |bibcode=2017MNRAS.470.3606H|s2cid=7301654|display-authors=29}} and the plane of the disk is likely misaligned with the planetary orbits by 17–32°.{{citation|arxiv=2010.02961|title=Mutual inclinations between giant planets and their debris discs in HD 113337 and HD 38529|year=2020|last1=Xuan|first1=Jerry W.|last2=Kennedy|first2=Grant M.|last3=Wyatt|first3=Mark C.|last4=Yelverton|first4=Ben|journal=Monthly Notices of the Royal Astronomical Society|volume=499|issue=4|pages=5059–5074|doi=10.1093/mnras/staa3155|doi-access=free |bibcode=2020MNRAS.499.5059X |s2cid=222177269}} The effective temperature of this disk is 55 K.{{citation|arxiv=1907.04800|title=A statistically significant lack of debris discs in medium separation binary systems|year=2019|doi=10.1093/mnras/stz1927|last1=Yelverton|first1=Ben|last2=Kennedy|first2=Grant M.|last3=Su|first3=Kate Y L.|last4=Wyatt|first4=Mark C.|journal=Monthly Notices of the Royal Astronomical Society|volume=488|issue=3|pages=3588–3606|doi-access=free |bibcode=2019MNRAS.488.3588Y|s2cid=195874349}}

The possibility of other stellar companions near the primary star was ruled out in 2016, for projected separations above 5″ (181 AU).{{citation|arxiv=1601.01524|title=A lucky imaging multiplicity study of exoplanet host stars II|year=2016|doi=10.1093/mnras/stw049|last1=Ginski|first1=C.|last2=Mugrauer|first2=M.|last3=Seeliger|first3=M.|last4=Buder|first4=S.|last5=Errmann|first5=R.|last6=Avenhaus|first6=H.|last7=Mouillet|first7=D.|last8=Maire|first8=A.-L.|last9=Raetz|first9=S.|journal=Monthly Notices of the Royal Astronomical Society|volume=457|issue=2|pages=2173–2191|doi-access=free |bibcode=2016MNRAS.457.2173G|s2cid=53626523}}

The existence of a secondary companion (called LDS 2662 B, or LSPM J1301+6337) was discovered in 2001{{citation|arxiv=1205.4718|title=The AstraLux Large M-dwarf Multiplicity Survey|year=2012|doi=10.1088/0004-637X/754/1/44|last1=Janson|first1=Markus|last2=Hormuth|first2=Felix|last3=Bergfors|first3=Carolina|last4=Brandner|first4=Wolfgang|last5=Hippler|first5=Stefan|last6=Daemgen|first6=Sebastian|last7=Kudryavtseva|first7=Natalia|last8=Schmalzl|first8=Eva|last9=Schnupp|first9=Carolin|last10=Henning|first10=Thomas|journal=The Astrophysical Journal|volume=754|issue=1|page=44|bibcode=2012ApJ...754...44J|s2cid=118475425}} and confirmed to be bound to the primary in 2007. Initially believed to be a single red dwarf star,{{citation|arxiv=astro-ph/0609555|title=Characterization of Dusty Debris Disks: The IRAS and Hipparcos Catalogs|year=2007|doi=10.1086/509912|last1=Rhee|first1=Joseph H.|last2=Song|first2=Inseok|last3=Zuckerman|first3=B.|last4=McElwain|first4=Michael|journal=The Astrophysical Journal|volume=660|issue=2|pages=1556–1571|bibcode=2007ApJ...660.1556R|s2cid=11879505}} in 2012 the companion was discovered to actually be a pair of nearly identical red dwarfs, of spectral class M3.5, orbiting each other at a distance of 7.2{{±|2.6}} AU, with a period of 39 years.