HD 147379

{{use dmy dates|date=January 2025}} {{short description|Visual binary in constellation Draco}} {{Starbox begin}} {{Starbox image | image= {{Location mark |image=Draco constellation map.svg|alt=|float=center|width=280 |label=|position=right |mark=Red circle.svg|mark_width=10|mark_link=HD 147379 |x=526|y=666 }} | caption=Location of HD 147379 (circled) }} {{Starbox observe 2s |epoch=J2000 |constell=[[Draco (constellation)|Draco]]<ref name=xhip/><ref name=xhipb/> |component1=HD 147379A |ra1={{RA|16|16|42.74635}}<ref name="DR3"/> |dec1={{DEC|+67|14|19.8316}}<ref name="DR3"/> |appmag_v1=8.9<ref name=Stalport2023/> |component2=HD 147379B |ra2={{RA|16|16|45.31448}}<ref name="DR3_B"/> |dec2={{DEC|+67|15|22.4811}}<ref name="DR3_B"/> |appmag_v2=10.69-10.74<ref name=Kazarovets1997/> }} {{Starbox character |component=HD 147379A |type=[[main sequence]]<ref name="DR3"/> |class=M0.0V<ref name=Stalport2023/> |b-v=1.11<ref name=Stalport2023/> |j-h=0.643<ref name=2MASS/> |j-k=0.826<ref name=2MASS/> |component2=HD 147379B |class2=M3V<ref name=Lehmann2023/> |j-h2=0.608<ref name=2MASS/> |j-k2=0.842<ref name=2MASS/> |variable2=[[BY Draconis variable]]<ref name=Kazarovets1997/> }} {{Starbox astrometry |component1=HD 147379A |radial_v={{val|-18.962|0.0011}}<ref name=DR2/> |prop_mo_ra=−497.915<ref name="DR3"/> |prop_mo_dec=84.047<ref name="DR3"/> |parallax=92.8766 |p_error=0.0146 |parallax_footnote=<ref name="DR3"/> |absmag_v=+8.47<ref name=xhip/> |component2=HD 147379B |radial_v2={{val|-18.36|0.0008}}<ref name=Fouque2018/> |prop_mo_ra2=−483.006<ref name="DR3_B"/> |prop_mo_dec2=89.049<ref name="DR3_B"/> |parallax2=92.8985 |p_error2=0.0160 |parallax_footnote2=<ref name="DR3_B"/> |absmag_v2=+10.54<ref name=xhipb/> }} {{Starbox orbit |reference=<ref name=Stalport2023/> |primary=HD 147379A |name=HD 147379B |period= |axis=64.4 |axis_unitless={{val|693.4|ul=AU}} |node= |periastron= |eccentricity= |inclination= |periarg= |k1= |k2= }} {{Starbox detail |source=<ref name=Reiners2018/> |component1=HD 147379A |mass={{val|0.58|0.08}} |radius={{val|0.57|0.06}} |luminosity={{val|0.1069|0.0153}}<ref name=Hobson2018/> |gravity={{val|4.609|0.012}}<ref name=Stalport2023/> |metal_fe={{val|0.16|0.16}} |temperature={{val|4090|50}} |rotational_velocity= |rotation={{val|22|ul=d}}<ref name=Pepper2018/> |age_gyr={{val|5.1|3.2|2.4}}<ref name=Veyette2018/> |component2=HD 147379B |mass2={{val|0.45|0.02}}<ref name=Lehmann2023/> |radius2={{val|0.460|0.008}}<ref name=Lehmann2023/> |luminosity2={{val|0.02645|0.00645}}<ref name=Stassun2019/> |gravity2={{val|4.84|0.06}}<ref name=Lehmann2023/> |metal_fe2={{val|0.20|0.10}}<ref name=Lehmann2023/> |temperature2={{val|3525|31}}<ref name=Lehmann2023/> |rotational_velocity2=0.50<ref name=Lehmann2023/> |rotation2={{val|40.4|3.0|ul=d}}<ref name=Lehmann2023/> }} {{Starbox catalog |names={{odlist|HD=147379|WDS=J16167+6714|GJ=617}} |component1=HD 147379A |names1={{odlist|2MASS=J16164280+6714196|AG=+67°695|BD=+67°935|G=257-32, G 225-57, G 240-14|GC=21949|HIP=79755|LHS=3175|LSPM=J1616+6714|LTT=14863|NLTT=42488|TIC=230073581|TYC=4195-721-1|UCAC4=787-024322|WISEA=J161641.85+671420.6|Gaia DR3=1642641410934267008}}<ref name="SIMBAD"/> |component2=HD 147379B |names2={{odlist|2MASS=J16164537+6715224|G=240-15, G 225-58, G 257-33|GSC=04195-01167|HIP=79762|LHS=3176|LSPM=J1616+6715|LTT=14864|NLTT=42489|PPM=19804|SAO=17026|TIC=230073588|TYC=4195-1167-1|UCAC4=787-024324|WISEA=J161644.44+671523.3|Gaia DR3=1642642957122493824|V=EW Draconis}}<ref name="SIMBAD_B"/> }} {{Starbox reference |Simbad=HD+147379|sn=A |Simbad2=HD+147379B|sn2=B }} {{Starbox end}} '''HD 147379''' ('''Gliese 617''') is a wide [[visual binary]] between two [[red dwarf]]s in the deep northern [[constellation]] of [[Draco (constellation)|Draco]]. The two stars are located approximately {{convert|35.1|ly|pc}} distant based on [[Gaia DR3]] [[Stellar parallax|parallax]] measurements, and approaching the [[Solar System]] at heliocentric [[Radial velocity|radial velocities]] of −18.962 km/s and −18.36 km/s, respectively. The brighter primary star, HD 147379A, has an [[apparent magnitude]] of 8.9,<ref name=Stalport2023/> too faint to be seen by the [[naked eye]] from [[Earth]] but visible using [[binoculars]].<ref name=bino/> The dimmer secondary, B, fluctuates in apparent magnitude between 10.69 and 10.74,<ref name=Kazarovets1997/> making it observable via a [[telescope]] with an [[aperture]] of 35 mm or larger.<ref name=North2014/>

==HD 147379A== HD 147379A (HIP 79755) is a red dwarf with a [[Stellar classification|spectral type]] of M0.0V, about 58% the [[Solar mass|mass of the Sun]], 57% the [[Solar radius|radius]], and an age of {{val|5.1|3.2|2.4|ul=billion years}}. It emits just over a tenth of the [[Solar luminosity|luminosity of the Sun]] from its [[photosphere]] at an [[effective temperature]] of {{convert|4090|K|C F}}. It has a high [[metallicity]] of [Fe/H]={{val|0.16|0.16|u=[[Metallicity#Chemical abundance ratios|dex]]}}, meaning it has an [[iron]] content somewhere around 45% higher than the Sun.<ref name=Reiners2018/> It is also enriched in [[cobalt]], but is depleted in [[calcium]] and [[titanium]]. The star shows slight variations in the [[Titanium(II) oxide|TiO]] [[spectral line]]s.<ref name=Zboril2009/>

===Planetary system=== In 2018, two teams independently reported the discovery of an [[exoplanet]] orbiting HD 147379A, both via the [[radial-velocity method]].<ref name=Reiners2018/><ref name=Hobson2018/> This was the first exoplanet found by the [[CARMENES survey]].<ref name=Reiners2018/> The planet, commonly referred to as HD 147379 b, has a [[minimum mass]] of 21.6 ± 1.1 {{Earth mass|sym=y|link=y}}, slightly more massive than [[Neptune]] (17.147 {{Earth mass|sym=y}}<ref name=Neptune/>). It orbits its host star once every 86.58 days at about a third of the distance from Earth to the Sun, placing it within the conservative [[habitable zone]] of the star, where [[Extraterrestrial liquid water#Extrasolar habitable zone candidates for water|liquid water]] could exist.<ref name=Stalport2023/>

One of the teams that discovered HD 147379 b proposed another candidate planet, this one with a minimum mass of 27 {{Earth mass|sym=y}} and a 500-day period, orbiting at a distance of about 1 AU.<ref name=Hobson2018/> However, a 2023 follow-up study did not detect such a signal. Instead, they detected a signal with a 12.3-day period, but discarded it due to the high chance of it being a false positive. Nevertheless, it is highly likely that a second planet exists interior to b's orbit.<ref name=Stalport2023/> {{OrbitboxPlanet begin | name = HD 147379A | table_ref = <ref name=Stalport2023/> }} {{OrbitboxPlanet | exoplanet = b | mass_earth = ≥21.6 ± 1.1 | period = 86.58 ± 0.14 | semimajor = 0.3315 ± 0.0024<ref name=Rosenthal2021/> | eccentricity = 0.0630{{±|0.0470|0.0380}} | radius_earth = | inclination = }} {{Orbitbox end}}

==HD 147379B== [[File:EWDraLightCurve.png|thumb|left|A [[Photometric system#Photometric letters|red-light]] [[light curve]] plotted from [[Zwicky Transient Facility|ZTF]] data<ref name="IRSA"/>]] HD 147379B (HIP 79762) is a [[Gravitational binding energy|gravitationally bound]] companion to HD 147379A at a separation of 64.4 [[arcsecond]]s, which corresponds to a distance of 693.4 AU.<ref name=Stalport2023/>

This is a red dwarf with a spectral type of M3V, about 45% the mass of the Sun and 46% the radius. It has a "partially convective" structure, meaning that the outer [[convection zone]] does not reach down to the [[Stellar core|core]],<ref name=Lehmann2023/> as opposed to "fully convective" stars weighing less than 0.35 {{Solar mass}} that are convective throughout.<ref name=Reiners2009/> It too has a high metallicity of [M/H]={{val|0.20|0.10|u=dex}}, translating to a roughly 60% excess in elements heavier than hydrogen and helium compared to the [[Sun]]. At an effective temperature of {{convert|3525|K|C F}},<ref name=Lehmann2023/> it radiates just 2.6% the luminosity of the Sun from its photosphere.<ref name=Stassun2019/> It [[Stellar rotation|rotates]] on its axis once every 40.4 days at a relatively slow projected equatorial velocity of 0.50 km/s.<ref name=Lehmann2023/>

It has a [[Stellar magnetic field|magnetic field]] that fluctuated in strength between 36-75 [[Gauss (unit)|G]] between 2020-2022, approximately 100 times stronger than [[Earth's magnetic field]] (0.22-0.67 G<ref name=geomag/>) and similar to those of faster-rotating red dwarfs. The variations in strength are smaller than those seen in fully convective red dwarfs such as [[Gliese 1151]].<ref name=Lehmann2023/>

In 1994, the star was reported to have a high likelihood (99%) of exhibiting long-term [[Variable star|variability]], albeit the author noted that this may be suspect.<ref name=Weis1994/> It was formally classified as a [[BY Draconis variable]] in 1997, receiving the [[variable-star designation]] EW Draconis.<ref name=Kazarovets1997/>

==References== <references>

<ref name=SIMBAD>{{cite simbad|title=HD 147379|access-date=2025-01-20}}</ref>

<ref name=SIMBAD_B>{{cite simbad|title=HD 147379B|access-date=2025-01-20}}</ref>

<ref name=North2014>{{cite book | title=Observing Variable Stars, Novae and Supernovae | first1=Gerald | last1=North | first2=Nick | last2=James | publisher=Cambridge University Press | date=2014 | isbn=978-1-107-63612-5 | page=24 | url=https://books.google.com/books?id=IzoDBAAAQBAJ&pg=PA24 }}</ref>

<ref name=geomag>{{Cite web |title=An Overview of the Earth's Magnetic Field |url=http://www.geomag.bgs.ac.uk/education/earthmag.html#_Toc2075549 |access-date=2024-03-02 |website=www.geomag.bgs.ac.uk}}</ref>

<ref name="bino">{{cite web |date=2004 |title=Limiting Magnitude in Binoculars |publisher=Cloudy Nights |first=Ed |last=Zarenski |url=http://www.cloudynights.com/documents/limiting.pdf |access-date=6 May 2011 |archive-url=https://web.archive.org/web/20110721072103/http://www.cloudynights.com/documents/limiting.pdf |archive-date=21 July 2011 |url-status=live }}</ref>

<ref name=Neptune>{{cite web |last=Williams |first=David R. |date=1 September 2004 |url=http://nssdc.gsfc.nasa.gov/planetary/factsheet/neptunefact.html |title=Neptune Fact Sheet |publisher=NASA |access-date=14 August 2007 |archive-url=https://web.archive.org/web/20100701192119/http://nssdc.gsfc.nasa.gov/planetary/factsheet/neptunefact.html |archive-date=1 July 2010 |url-status=live }}</ref>

<ref name="IRSA">{{cite web |title=NASA/IPAC Infrared Science Archive |url=https://irsa.ipac.caltech.edu/frontpage/ |website=IRSA |publisher=NASA |access-date=13 October 2025}}</ref>

<ref name=Reiners2009>{{cite journal | last1=Reiners | first1=Ansgar | last2=Basri | first2=Gibor | title=On the magnetic topology of partially and fully convective stars | journal=Astronomy and Astrophysics | volume=496 | issue=3 | pages=787–790 |date=March 2009 | doi=10.1051/0004-6361:200811450 | bibcode=2009A&A...496..787R |arxiv = 0901.1659 | s2cid=15159121 }}</ref>

<ref name=Lehmann2023>{{cite journal | display-authors=3 | last1=Lehmann | first1=L T | last2=Donati | first2=J-F | last3=Fouqué | first3=P | last4=Moutou | first4=C | last5=Bellotti | first5=S | last6=Delfosse | first6=X | last7=Petit | first7=P | last8=Carmona | first8=A | last9=Morin | first9=J | last10=Vidotto | first10=A A | author11=the SLS consortium | title=SPIRou reveals unusually strong magnetic fields of slowly rotating M dwarfs | journal=Monthly Notices of the Royal Astronomical Society | volume=527 | issue=2 | date=2023-11-09 | issn=0035-8711 | doi=10.1093/mnras/stad3472 | doi-access=free | pages=4330–4352 }}</ref>

<ref name=Weis1994>{{cite journal | last=Weis | first=Edward W. | title=Long term variability in dwarf M stars | journal=The Astronomical Journal | volume=107 | date=1994 | doi=10.1086/116925 | page=1135| bibcode=1994AJ....107.1135W }}</ref>

<ref name=Kazarovets1997>{{cite journal |last1=Kazarovets |first1=E. V. |last2=Samus |first2=N. N. |title=The 73rd Name-List of Variable Stars |journal=Information Bulletin on Variable Stars |date=23 April 1997 |volume=4471 |pages=1–45 |bibcode=1997IBVS.4471....1K }}</ref>

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</references> {{Draco (constellation)}} [[Category:Binary stars]] [[Category:Draco (constellation)]] [[Category:Henry Draper Catalogue objects|147379]] [[Category:Hipparcos objects|079755]] [[Category:Gliese and GJ objects|0617]] [[Category:M-type main-sequence stars]] [[Category:Planetary systems with one confirmed planet]] [[Category:Durchmusterung objects|BD+67 935]] [[Category:Objects with variable star designations|Draconis, EW]] [[Category:BY Draconis variables]] [[Category:Population I stars]]