HD 134606#Planetary system
{{Short description|Star in the constellation Apus}}
{{Starbox begin
| name = HD 134606
}}
{{Starbox observe
| epoch = J2000
| constell = Apus
| dec = {{DEC|−70|31|10.6449}}
}}
{{Starbox character
| type = subgiant
| u-b =
| variable =
}}
{{Starbox astrometry
| radial_v = {{val|+1.94|0.12}}
| prop_mo_ra = −177.871
| prop_mo_dec = −164.709
| parallax = 37.3020
| p_error = 0.0182
}}
{{Starbox detail
| mass = {{val|1.046|0.070|0.059}}
| radius = {{val|1.158|0.039|0.036}}
| luminosity = {{val|1.161|0.071|0.049}}
| gravity = {{val|4.330|0.044|0.041}}
| temperature = {{val|5576|86|85|fmt=commas}}
| metal_fe = {{val|+0.343|0.081|0.084}}
| rotation = {{val|42.0|3.9|ul=d}}
| rotational_velocity =
| age_gyr = {{val|7.3|3.6|3.4}}
}}
{{Starbox catalog
| names = {{odlist | CD=−70°1258 | HD=134606 | HIP=74653 | SAO=257257 | LTT=6064 | GC=20455|2MASS=J15151504-7031105}}
}}
{{Starbox reference
| Simbad = HD+134606
| NSTED = HD-134606
}}
{{Starbox end}}
HD 134606 is a yellow-hued star with a planetary system, positioned in the southern constellation of Apus. It is below the nominal limit for visibility with the naked eye, having an apparent visual magnitude of 6.86. Based upon an annual parallax shift of {{Val|37.3|ul=mas}}, it is located 87.44 light-years away. The star appears to be moving further from the Earth with a heliocentric radial velocity of +1.9 km/s.
This is an evolving G-type subgiant star with a stellar classification of G6 IV and is not considered magnetically active, having a chromospheric activity index of −5.04. It has about the same mass as the Sun but is 25% more luminous. The photosphere is radiating energy at an effective temperature of 5,614 K. It has a higher than solar metallicity – a term astronomers use to describe the abundance of elements other than hydrogen and helium.
There is a companion star of spectral type M3V at a separation of ~1500 AU, designated L 72-1. Analysis of its light curve indicate it is itself a close binary.
Planetary system
The discovery of a planetary system orbiting HD 134606 was announced in 2011, following an eight-year survey carried out at the La Silla Observatory in Chile. The detection was made via the radial velocity method using the HARPS instrument. Applying a Keplerian fit to the data suggested the presence of three planets in moderately eccentric orbits. None of the planetary orbits displays a mean motion resonance with the others.
The system was updated by a 2024 study, which confirmed the three previously reported planets, though with a longer period for planet d, and detected two new ones. While all five planets are very likely to be real, the study advises caution regarding planet f due to the similarity of its period to the lunar cycle. The five planets range from super-Earth to super-Neptune mass, and the outermost, HD 134606 d, is a small gas giant orbiting within the habitable zone that may be a candidate for future space-based direct imaging missions. A long-period radial velocity trend was also detected, suggesting the presence of a distant sixth substellar companion.
{{OrbitboxPlanet begin
}}
{{OrbitboxPlanet
| exoplanet = e
| mass_earth = {{val|2.34|0.35|0.34|p=≥}}
| period = {{val|4.3203|0.00051|0.00047}}
| semimajor = {{val|0.0527|0.0011|0.0012}}
| eccentricity = {{val|0.2|0.14|0.13}}
}}
{{OrbitboxPlanet
| exoplanet = b
| mass_earth = {{val|9.09|0.64|0.63|p=≥}}
| period = {{val|12.089|0.0016|0.0015}}
| semimajor = {{val|0.1046|0.0023|0.0024}}
| eccentricity = {{val|0.092|0.054|0.053}}
}}
{{OrbitboxPlanet
| exoplanet = f
| mass_earth = {{val|5.63|0.72|0.69|p=≥}}
| period = {{val|26.915|0.016}}
| semimajor = {{val|0.1784|0.0039|0.0041}}
| eccentricity = {{val|0.081|0.1|0.059}}
}}
{{OrbitboxPlanet
| exoplanet = c
| mass_earth = {{val|11.31|1.0|0.99|p=≥}}
| period = {{val|58.883|0.041|0.039}}
| semimajor = {{val|0.3007|0.0066|0.0069}}
| eccentricity = {{val|0.055|0.062|0.04}}
}}
{{OrbitboxPlanet
| exoplanet = d
| mass_earth = {{val|44.8|2.9|p=≥}}
| period = {{val|966.5|5.3|6.9}}
| semimajor = {{val|1.941|0.043|0.046}}
| eccentricity = {{val|0.092|0.045}}
}}
{{Orbitbox end}}
References
{{reflist|refs=
{{cite simbad | title=HD 134606 | access-date=October 20, 2018 }}
{{cite simbad | title=L 72-1 | access-date=1 February 2024}}
{{Cite Gaia DR3|5798962867668048768}}
| title=XHIP: An extended hipparcos compilation
| last1=Anderson | first1=E. | last2=Francis | first2=Ch.
| journal=Astronomy Letters
| volume=38 | issue=5 | pages=331 | year=2012
| bibcode=2012AstL...38..331A | doi=10.1134/S1063773712050015
| arxiv=1108.4971 | s2cid=119257644 | postscript=. }}
| title=An activity catalogue of southern stars
| last1=Jenkins | first1=J. S. | last2=Jones | first2=H. R. A.
| last3=Tinney | first3=C. G. | last4=Butler | first4=R. P.
| last5=McCarthy | first5=C. | last6=Marcy | first6=G. W.
| last7=Pinfield | first7=D. J. | last8=Carter | first8=B. D.
| last9=Penny | first9=A. J. | display-authors=1
| journal=Monthly Notices of the Royal Astronomical Society
| volume=372 | issue=1 | pages=163–173 | date=October 2006
| bibcode=2006MNRAS.372..163J | arxiv=astro-ph/0607336
| doi=10.1111/j.1365-2966.2006.10811.x | doi-access=free | s2cid=17524675 | postscript=. }}
| last1=Gray | first1=R. O. | last2=Corbally | first2=C. J.
| last3=Garrison | first3=R. F. | last4=McFadden | first4=M. T.
| last5=Bubar | first5=E. J. | last6=McGahee | first6=C. E.
| last7=O'Donoghue | first7=A. A. | last8=Knox | first8=E. R.
| title=Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample
| journal=The Astronomical Journal | display-authors=1
| volume=132 | issue=1 | pages=161–170 | date=July 2006
| doi=10.1086/504637 | arxiv=astro-ph/0603770
| bibcode=2006AJ....132..161G | s2cid=119476992 }}
{{cite journal | display-authors=1
| last1=Tsantaki | first1=M. | last2=Sousa | first2=S. G.
| last3=Adibekyan | first3=V. Zh. | last4=Santos | first4=N. C.
| last5=Mortier | first5=A. | last6=Israelian | first6=G.
| title=Deriving precise parameters for cool solar-type stars. Optimizing the iron line list
| journal=Astronomy & Astrophysics
| volume=555 | page=A150 | date=July 2013
| doi=10.1051/0004-6361/201321103
| arxiv=1304.6639 | bibcode=2013A&A...555A.150T | s2cid=118388752 }}
| first1=M. | last1=Mayor | first2=M. | last2=Marmier
| first3=C. | last3=Lovis | first4=S. | last4=Udry
| first5=D. | last5=Ségransan | first6=F. | last6=Pepe
| first7=W. | last7=Benz | first8=J.-L. | last8=Bertaux
| first9=F. | last9=Bouchy | first10=X. | last10=Dumusque
| first11=G. | last11=Lo Curto | first12=C. | last12=Mordasini
| first13=D. | last13=Queloz | first14=N. C. | last14=Santos
| title=The HARPS search for southern extra-solar planets XXXIV. Occurrence, mass distribution and orbital properties of super-Earths and Neptune-mass planets
| date=September 13, 2011 | arxiv=1109.2497 }}
| title=A semi-empirical stability criterion for real planetary systems with eccentric orbits
| last1=Giuppone | first1=C. A. | last2=Morais | first2=M. H. M.
| last3=Correia | first3=A. C. M. | display-authors=1
| journal=Monthly Notices of the Royal Astronomical Society
| volume=436 | issue=4 | pages=3547–3556 | date=December 2013
| doi=10.1093/mnras/stt1831 | doi-access=free | bibcode=2013MNRAS.436.3547G | arxiv=1309.6861 }}
{{cite journal |last1=Li |first1=Zhexing |last2=Kane |first2=Stephen R. |last3=Brandt |first3=Timothy D. |last4=Fetherolf |first4=Tara |last5=Robertson |first5=Paul |last6=Zhao |first6=Jinglin |last7=Dalba |first7=Paul A. |last8=Wittenmyer |first8=Robert A. |last9=Butler |first9=R. Paul |date=April 2024 |title=Revised Architecture and Two New Super-Earths in the HD 134606 Planetary System |journal=The Astronomical Journal |volume=167 |issue=4 |pages=155 |doi=10.3847/1538-3881/ad2461 |doi-access=free |arxiv=2401.17415 |bibcode=2024AJ....167..155L}}
}}
{{Stars of Apus}}
{{DEFAULTSORT:HD 134606}}