{{Short description|Young star in the constellation of Lupus}} {{Starbox begin |name=HD 142527}} {{Starbox image |image=[[File:Artist’s impression of the disc and gas streams around HD 142527.jpg|250px]] |caption=Artist’s impression of the disc and gas streams around HD 142527 }} {{Starbox observe |constell=[[Lupus (constellation)|Lupus]]<ref>{{cite constellation|HD 142527}}</ref> |epoch=[[J2000]] | ra = {{RA|15|56|41.88986}}<ref name="van Leeuwen2007">{{cite journal | title=Validation of the new Hipparcos reduction | last1=van Leeuwen | first1=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}} [http://webviz.u-strasbg.fr/viz-bin/VizieR-5?-out.add=.&-source=I/311/hip2&recno=14774 Vizier catalog entry ]</ref> | dec = {{DEC|-42|19|23.2746}}<ref name="van Leeuwen2007"/> |appmag_v=8.34<ref name="SIMBAD">{{cite simbad|title=HD 142527|accessdate=5 January 2017}}</ref> }} {{Starbox character |class=F6 III<ref name="SIMBAD"/> }} {{Starbox astrometry |radial_v=-3.10<ref name="SIMBAD" /> |prop_mo_ra=-11.19<ref name="van Leeuwen2007"/> |prop_mo_dec=-24.46<ref name="van Leeuwen2007"/> |parallax=6.2791 |p_error=0.0284 |parallax_footnote=<ref>{{cite Gaia EDR3|5994826707951507200}}</ref> |absmag_v= }} {{Starbox orbit | reference = <ref name=Nowak2024>{{cite journal | doi=10.1051/0004-6361/202347748| title=The orbit of HD 142527 B is too compact to explain many of the disc features | year=2024| last1=Nowak| first1=M. | last2=Rowther| first2=S. | last3=Lacour | first3=S.| last4=Meru | first4=F.| last5=Nealon | first5=R. | last6=Price | first6=D. J. | journal=Astronomy & Astrophysics | volume=683 | pages=A6 | arxiv=2402.03595| bibcode=2024A&A...683A...6N | doi-access=free}}</ref> | primary = HD 142527 A | name = HD 142527 B | period = 23.50{{±|0.85}} | period_unitless = <!--(P) Period (no units provided by template)--> | axis = 0.0678{{±|0.014}} | axis_unitless = 10.80{{±|0.22}} [[astronomical unit|AU]] | eccentricity = 0.47{{±|0.01}} | inclination = 149.47{{±|0.71}} | node = 161.51{{±|2.01}} | periastron = 2020.42{{±|0.05}} | periarg = 186.45{{±|0.48}} | periarg_primary = <!--(ω) Argument of periapsis (in degrees), primary --> | k1 = <!-- Velocity semi-amplitude (SB1, or primary in SB2), in km/s --> | k2 = <!-- Velocity semi-amplitude (secondary in SB2), in km/s --> }} {{Starbox detail | component1=HD 142527 A | mass=2.2{{±|0.05}}<ref name=Guzman-Diaz2021>{{cite journal | title=Homogeneous study of Herbig Ae/Be stars from spectral energy distributions and ''Gaia'' EDR3 | last1=Guzmán-Díaz | first1=J. | last2=Mendigutía | first2=I. | last3=Montesinos | first3=B. | last4=Oudmaijer | first4=R. D. | last5=Vioque | first5=M. | last6=Rodrigo | first6=C. | last7=Solano | first7=E. | last8=Meeus | first8=G. | last9=Marcos-Arenal | first9=P. | year=2021 | journal=Astronomy & Astrophysics | volume=650 | pages=A182 | bibcode=2021A&A...650A.182G | doi=10.1051/0004-6361/202039519 | arxiv=2104.11759 | doi-access=free}}</ref> | age_myr=4.4{{±|0.49|0.38}}<ref name=Guzman-Diaz2021/> | radius=3.46{{±|0.13}}<ref name=Guzman-Diaz2021/> | luminosity=22.39{{±|0.52}}<ref name=Guzman-Diaz2021/> | temperature=6632<ref name=Luck>{{cite journal|title=Abundances in the Local Region. I. G and K Giants | author=Luck, R. Earle | date=2015 | journal=The Astronomical Journal | volume=150 | issue=3 | page=88 | bibcode=2015AJ....150...88L | doi=10.1088/0004-6256/150/3/88 | arxiv=1507.01466 | s2cid=118505114}}</ref> | gravity=3.15<ref name=Luck/> | metal_fe=0.33<ref name=Luck/> | component2=HD 142527 B | mass2=0.34{{±|0.06}}<ref name=Christiaens2018>{{cite journal | title=Characterization of low-mass companion HD 142527 B | last1=Christiaens | first1=V. | last2=Casassus | first2=S. | last3=Absil | first3=O. | last4=Kimeswenger | first4=S. | last5=Gomez Gonzalez | first5=C. A. | last6=Girard | first6=J. | last7=Ramírez | first7=R. | last8=Wertz | first8=O. | last9=Zurlo | first9=A. | last10=Wahhaj | first10=Z. | last11=Flores | first11=C. | last12=Salinas | first12=V. | last13=Jordán | first13=A. | last14=Mawet | first14=D. | year=2018 | journal=Astronomy & Astrophysics | volume=617 | pages=A37 | bibcode=2018A&A...617A..37C | doi=10.1051/0004-6361/201629454 | arxiv=1806.04792 | doi-access=free}}</ref> | radius2=1.37{{±|0.05}}<ref name=Christiaens2018/> | luminosity2=0.25{{±|0.04}}<ref name=Christiaens2018/> | temperature2=3500{{±|100}}<ref name=Christiaens2018/> | age_myr2=1.8{{±|1.2|-0.5}}<ref name=Christiaens2018/> }} {{Starbox catalog |names= [[Cordoba Durchmusterung|CD]]−41°10447, [[Henry Draper Catalogue|HD]] 142527, [[Hipparcos catalogue|HIP]] 78092, [[Smithsonian Astrophysical Observatory Star Catalog|SAO]] 226389, [[Washington Double Star Catalog|WDS]] J15567-4219AB, [[2MASS]] J15564188-4219232, TYC 846-688-1, Gaia DR2 5994826707951507200<ref name="SIMBAD" /> }} {{Starbox reference |Simbad=HD+142527 }} {{Starbox end}} [[File:HD142527LightCurve.png|thumb|right|A [[Photometric system#Photometric letters|visual band]] [[light curve]] for HD 142527, plotted from ''[[All Sky Automated Survey for SuperNovae|ASAS-SN]]'' data<ref name="ASAS-SN">{{cite web |url=https://asas-sn.osu.edu/variables/lookup |website=ASAS-SN Variable Stars Database|title=ASAS-SN Variable Stars Database|publisher=ASAS-SN |access-date=6 January 2022}}</ref>]]
'''HD 142527''' is a [[binary star]] system in the [[Lupus (constellation)|constellation of Lupus]].<ref>{{Cite web|url=http://simbad.u-strasbg.fr/simbad/sim-id?Ident=HD+142527|title = Hd 142527}}</ref><ref name=casassus2013>{{cite journal |bibcode=2013Natur.493..191C |title=Flows of gas through a protoplanetary gap |last1=Casassus |first1=Simon |last2=Van Der Plas |first2=Gerrit M. |last3=Perez |first3=Sebastian |last4=Dent |first4=William R. F. |last5=Fomalont |first5=Ed |last6=Hagelberg |first6=Janis |last7=Hales |first7=Antonio |last8=Jordán |first8=Andrés |last9=Mawet |first9=Dimitri |last10=Ménard |first10=Francois |last11=Wootten |first11=Al |last12=Wilner |first12=David |last13=Hughes |first13=A. Meredith |last14=Schreiber |first14=Matthias R. |last15=Girard |first15=Julien H. |last16=Ercolano |first16=Barbara |last17=Canovas |first17=Hector |last18=Román |first18=Pablo E. |last19=Salinas |first19=Vachail |journal=Nature |date=2013 |volume=493 |issue=7431 |pages=191–194 |doi=10.1038/nature11769 |pmid=23283173 |arxiv=1305.6062 }}</ref> The primary star belongs to the [[Herbig Ae/Be star]] class, while the companion, discovered in 2012, is a [[red dwarf]] star or accreting protoplanet<ref name=Balmer2022>{{cite journal | doi=10.3847/1538-3881/ac73f4| title=Improved Orbital Constraints and Hα Photometric Monitoring of the Directly Imaged Protoplanet Analog HD 142527 B| year=2022| last1=Balmer| first1=William O.| last2=Follette| first2=Katherine B.| last3=Close| first3=Laird M.| last4=Males| first4=Jared R.| last5=De Rosa| first5=Robert J.| last6=Adams Redai| first6=Jéa I.| last7=Watson| first7=Alex| last8=Weinberger| first8=Alycia J.| last9=Morzinski| first9=Katie M.| last10=Morales| first10=Julio| last11=Ward-Duong| first11=Kimberly| last12=Pueyo| first12=Laurent| journal=The Astronomical Journal| volume=164| issue=1| page=29| arxiv=2206.00687| bibcode=2022AJ....164...29B| s2cid=249282495| doi-access=free}}</ref> with a projected separation of less than 0.1″.<ref name=Hunziker2021>{{citation|arxiv=2103.08462|year=2021|title=HD 142527: Quantitative disk polarimetry with SPHERE|doi=10.1051/0004-6361/202040166|last1=Hunziker|first1=S.|last2=Schmid|first2=H. M.|last3=Ma|first3=J.|last4=Menard|first4=F.|last5=Avenhaus|first5=H.|last6=Boccaletti|first6=A.|last7=Beuzit|first7=J. L.|last8=Chauvin|first8=G.|last9=Dohlen|first9=K.|last10=Dominik|first10=C.|last11=Engler|first11=N.|last12=Ginski|first12=C.|last13=Gratton|first13=R.|last14=Henning|first14=T.|last15=Langlois|first15=M.|last16=Milli|first16=J.|last17=Mouillet|first17=D.|last18=Tschudi|first18=C.|last19=Van Holstein|first19=R. G.|last20=Vigan|first20=A.|journal=Astronomy & Astrophysics|volume=648|pages=A110|bibcode=2021A&A...648A.110H|s2cid=232233697}}</ref> The system is notable for its circumbinary protoplanetary disk and its discovery has helped refine models of planet formation. The orbit of companion is strongly inclined to the circumbinary protoplanetary disk.<ref name=Balmer2022/> A possible second companion was discovered in 2026.<ref>{{Citation |last=Tran |first=T. M. H. |title=Exploration of the inner region of the system HD 142527 |date=2026-05-06 |url=http://arxiv.org/abs/2605.04869 |access-date=2026-05-10 |publisher=arXiv |doi=10.48550/arXiv.2605.04869 |id=arXiv:2605.04869 |last2=Langlois |first2=M. |last3=Flasseur |first3=O. |last4=Augereau |first4=J.-C. |last5=Boccaletti |first5=A. |last6=Delorme |first6=P. |last7=Gratton |first7=R. |last8=Kaszczyc |first8=A. |last9=Lagrange |first9=A.-M.}}</ref>
HD 142527 is listed in the International Variable star index as a UX Orionis variable, with a visible-light magnitude ranging from 8.27 to 8.60.<ref name="IVSI">{{cite web |title=NSV 20441 |url=https://www.aavso.org/vsx/index.php?view=detail.top&oid=58876 |website=The International Variable Star Index |publisher=AAVSO |access-date=10 November 2022}}</ref>
==Protoplanetary disk== HD 142527 is an extremely young [[star system]], aged about 4.4 million years old<ref name=Guzman-Diaz2021/> so it retains its [[protoplanetary disk]], which has a [[mass]] of 15 [[percent|%]] of [[solar mass|the Sun]] and a diameter of 980 [[Astronomical Unit|AU]].
Studies have shown eddies and vortex structures forming in the disk under the influence of two large [[planet]]s.<ref name=casassus2013/> The system is important as it allows [[astronomer]]s to observe the accretion process in [[planet formation|planetary formation]].
In early 2013 an article was published by astronomers working with the ALMA telescope in [[Chile]], which refers to the discovery of two massive flows of matter in the system.<ref name=casassus2013/> Dust and gas is transferred from the periphery to the center through gravitational interaction with two giant planets that have a mass several times greater than the mass of [[Jupiter]]. Thus, the flows act as "pumps", pumping material from the edge of the center, "feeding" star. The planets themselves have not been detected so far, due to a dense shroud of gas. However, astronomers have proposed models that describe their existence.
[[Japan]]ese [[astronomer]]s have discovered particles of [[water|ice]]<ref>{{cite journal |bibcode=2009ApJ...690L.110H |title=Detection of Water Ice Grains on the Surface of the Circumstellar Disk Around HD 142527 |last1=Honda |first1=M. |last2=Inoue |first2=A. K. |last3=Fukagawa |first3=M. |last4=Oka |first4=A. |last5=Nakamoto |first5=T. |last6=Ishii |first6=M. |last7=Terada |first7=H. |last8=Takato |first8=N. |last9=Kawakita |first9=H. |last10=Okamoto |first10=Y. K. |last11=Shibai |first11=H. |last12=Tamura |first12=M. |last13=Kudo |first13=T. |last14=Itoh |first14=Y. |journal=The Astrophysical Journal |date=2009 |volume=690 |issue=2 |pages=L110–L113 |doi=10.1088/0004-637X/690/2/L110 }}</ref> in the disk. {{OrbitboxPlanet begin | name = <!--Name of star (only use if article title differs from planet host star name)---> | table_ref = <ref name=Hunziker2021/> | period_unit = day }} {{OrbitboxPlanet disk | disk = [[protoplanetary disk]] | periapsis = 140 | apoapsis = 550 | inclination = 28 }} {{Orbitbox end}}
==References== {{reflist}}
{{Stars of Lupus}}
[[Category:Lupus (constellation)]] [[Category:Binary stars]] [[Category:Herbig Ae/Be stars]] [[Category:Henry Draper Catalogue objects|142527]] [[Category:Hipparcos objects|078092]] [[Category:Durchmusterung objects|CD-41 10447]] [[Category:Circumstellar disks]] [[Category:F-type giants]]