HD 53705/53706/53680 is a star system that lies approximately 54 light-years away in the constellation of Puppis. The system consists of four stars in two binaries, making it one of the nearest quadruple star systems.
 | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Puppis |
| HD 53705 | |
| Right ascension | 07h 03m 57.317s ± 11.59[1] |
| Declination | −43° 36′ 28.94″ ± 2.46[1] |
| Apparent magnitude (V) | 5.7033 ± 0.0320[1] |
| HD 53706 | |
| Right ascension | 07h 03m 58.911s ± 110.53[1] |
| Declination | −43° 36′ 40.56″ ± 79.27[1] |
| Apparent magnitude (V) | 7.0459 ± 0.0908[1] |
| HD 53680 | |
| Right ascension | 07 03h 50.236m ± 12.82[1] |
| Declination | −43° 33′ 40.82″ ± 8.53[1] |
| Apparent magnitude (V) | 8.8041 ± 0.0017 |
| Characteristics | |
| HD 53705 A | |
| Spectral type | G0V |
| B−V color index | 0.624 ± 0.009 |
| HD 53706 B | |
| Spectral type | K0V |
| B−V color index | 0.779 ± 0.020 |
| HD 53680 AB | |
| Spectral type | K5V/M(MS) |
| B−V color index | 1.180 ± 0.012 |
| Astrometry | |
| HD 53705 A | |
| Radial velocity (Rv) | 89.5[2] km/s |
| Proper motion (μ) | RA: -104.10 ± 0.91[1] mas/yr Dec.: 389.07 ± 1.32[1] mas/yr |
| Parallax (π) | 60.55 ± 1.04 mas[1] |
| Distance | 53.9 ± 0.9 ly (16.5 ± 0.3 pc) |
| HD 53706 B | |
| Radial velocity (Rv) | 89.0[2] km/s |
| Proper motion (μ) | RA: -113.80 ± 9.01[1] mas/yr Dec.: 417.98 ± 12.58[1] mas/yr |
| Parallax (π) | 47.99 ± 9.89 mas[1][note 1] |
| Distance | 68.0 ± 14.6 ly (20.8 ± 4.5 pc) |
| HD 53680 AB | |
| Radial velocity (Rv) | 89.065 ± 0.005[3] km/s |
| Proper motion (μ) | RA: -75.64 ± 0.97[1] mas/yr Dec.: 393.50 ± 1.46[1][note 2] mas/yr |
| Parallax (π) | 58.2 ± 0.8 mas[3] |
| Distance | 56.0 ± 0.8 ly (17.2 ± 0.2 pc) |
| Absolute magnitude (MV) | 7.81 ± 0.03[4] |
| Orbit[3] | |
| Primary | HD 53680 A |
| Companion | HD 53680 B |
| Period (P) | 1688.6 ± 1.1 days |
| Semi-major axis (a) | 34.9 ± 3.2 mas |
| Eccentricity (e) | 0.475 ± 0.002 |
| Inclination (i) | 163.6 +1.4 −1.7° |
| Longitude of the node (Ω) | 238.9 ± 2.9° |
| Argument of periastron (ω) (secondary) | -133.2 ± 0.3° |
| Semi-amplitude (K1) (primary) | 1.2398 +0.0041 −0.0040 km/s |
| Details | |
| HD 53705 | |
| Mass | 0.98 +0.02 −0.03[5] M☉ |
| Radius | 1.14 +0.04 −0.03[5] R☉ |
| Luminosity | 1.34 +0.11 −0.10 (log 0.127 ± 0.035)[2] L☉ |
| Surface gravity (log g) | 4.34 +0.03 −0.04[5] cgs |
| Temperature | 5827 ± 44[2] K |
| Metallicity [Fe/H] | -0.21 ± 0.03[2] dex |
| Rotational velocity (v sin i) | 1.6 ± 0.5[2] km/s |
| Age | 8.56 +1.44 −1.72[5] Gyr |
| HD 53706 | |
| Mass | 0.81 +0.04 −0.03[5] M☉ |
| Radius | 0.79 +0.03 −0.03[5] R☉ |
| Luminosity | 0.40 +0.25 −0.15 (log -0.40 ± 0.21)[2][note 3] L☉ |
| Surface gravity (log g) | 4.59 +0.03 −0.05[5] cgs |
| Temperature | 5245 ± 44[2] K |
| Metallicity [Fe/H] | -0.28 ± 0.03[2] dex |
| Rotational velocity (v sin i) | 0.3 ± 0.5[2] km/s |
| Age | 11.7 +3.3 −9.6 (weakly constrained)[2] Gyr |
| HD 53680 AB | |
| Mass | 0.79 ± 0.02 / 0.22 ± 0.02[3][note 4] M☉ |
| Radius | 0.64 ± 0.05[4] R☉ |
| Temperature | 4460 ± 100[4] K |
| Metallicity [Fe/H] | -0.29 ± 0.08[3] dex |
| Rotational velocity (v sin i) | 2.08 ± 0.31[3] km/s |
| Age | 0.7 - 9.4 (weakly constrained)[3] Gyr |
| Other designations | |
| HD 53705: HD 53705, HIP 34065, HR 2667 | |
| HD 53706: HD 53706, HIP 34069, HR 2668 | |
| HD 53680: HD 53680, HIP 34052 | |
| Database references | |
| HD 53705 | |
| SIMBAD | data |
| HD 53706 | |
| SIMBAD | data |
| HD 53680 AB | |
| SIMBAD | data |
Component discovery
edit
HD 53705 was discovered to be a visual binary very early on, owing to the brightness of the two components. The earliest observation in the Washington Double Star Catalog (WDS) dates to 1826 and was made by James Dunlop, stating a position angle of 119 degrees and a separation of 21.5 arcseconds for the companion.[6] The two stars have moved very little relative to each other since, with the most recent measurement from 1999 stating a position angle of 126 degrees and a separation of 20.9 arcseconds. This is related to the nearby location of the system: a separation of 21 arcseconds translates to a physical separation perpendicular to the line of sight of approximately 480 AU,[7] so the orbit of the stars lasts somewhere on the order of millennia.
The companionship of HD 53680 to the closer binary was recognised later, with the first measurement in the WDS dating to 1900.[6] With a position angle of 337 degrees and a separation of 185.7 arcseconds, HD 53680 lies on the opposite side of HD 53705 when compared to B, and is about nine times more distant. This separation results in a physical separation perpendicular to the line of sight of 4390 AU,[7] which is atypically distant for a stellar companion but still close enough to be strongly gravitationally bound.
While all three components have similar proper motion, HD 53680's proper motion as measured by HIPPARCOS is sizeably discrepant from the proper motions of the other two components. A clue to the cause of this is that HD 53680's Tycho-2 proper motion is different from the HIPPARCOS values, which indicates that the star is being perturbed by a close companion.[8] A fit of the HIPPARCOS astrometric data found a weakly constrained fit found a period of 1500 days, an inclination of 180 degrees (a face-on orbit) and a semimajor axis of 30.6 milliarcseconds.[9] The fit is weakly constrained because HIPPARCOS observations do not span the full orbit of the companion, but the fit does adjust HD 53680's proper motion to be consistent with the proper motion of HD 53705/53706.
The low inclination of HD 53680 B's orbit reduces the amplitude of the radial velocity variation that it caused on HD 53680 A. In this case, the effect reduced the minimum mass of the companion into the brown dwarf regime as deduced from observations with the CORALIE spectrograph.[3] The spectroscopic orbit produces far stronger constraint compared to the astrometry-only orbit.
Stellar properties
editHD 53705, with a spectral type of G0V, is a G-type main-sequence star that is slightly hotter, larger and brighter than the Sun. Meanwhile, HD 53706 and HD 53680 A are both K-type main-sequence stars, with spectral types of K0V and K5V, respectively. Both of these stars are substantially cooler, smaller and dimmer than the Sun.
The three stars with observed spectra in the system have similar metallicity values: [Fe/H] = -0.21 ± 0.03 and -0.28 ± 0.03 for HD 53705 and B,[2] and [Fe/H] = -0.29 ± 0.08 for HD 53680 A.[3] The average value, -0.26 ± 0.04, results in an iron abundance of 55 ± 5% solar, a value typical for field stars.
The sub-solar metallicity of the stars has the effect of heating up their chromospheres; Though HD 53705 has a mass that is approximately solar, its effective temperature is about fifty degrees hotter.[citation needed]
The kinematics of the stars, with large proper motion and radial velocity, suggests that the system is a member of the thick disk,[7][9] the population of stars that comprise most of the older members of the Milky Way's spiral arms. This is supported by the parameters of HD 53705; the surface gravity of 4.34 is somewhat low for a G0V star, indicating that it is relatively old and moving towards the end of its main sequence lifetime - which, when coupled with the solar mass, mean that estimates for the star's age are approximately 9 billion years old, approximately twice the solar age. With a peculiar velocity of 75.7 km/s, The orbit of the system about the galaxy has an eccentricity of 0.31 and brings the system up to 151 parsecs away from the galactic plane - again indicative of a thick disk system.[7]
Planet searches
editBeing bright, solar-type and nearby, HD 53705 and B are attractive targets for radial velocity (RV)-based planet searches.
HD 53705 was one of the 37 targets of the first RV-based planet search in the southern hemisphere, the ESO CES survey.[10] This survey did not detect any companion with several Jovian masses out to a few AU. An extension of this survey to the HARPS spectrograph provides further constraint, suggesting that there are no Jupiter-mass companions out to about 5 AU.[11]
HD 53705 can be presumed to be on the CORALIE sample, as it satisfies the criteria of parallax = ≥20 mas with error ≤5 mas, and spectral type between F8 and M1.[12] HD 53706 fails the criteria due to the large error on its parallax, while HD 53680 satisfies them.[3]
The two stars are also on the Anglo-Australian Telescope sample,[13] which has found that they are stable to 4.5 and 2.9 m/s, respectively. This excludes the presence of giant planets at separations of a few AU around either star.[14]
Notes
edit- ^ The poor quality of HD 53706's HIPPARCOS data is due to being in such close vicinity to HD 53705; the light from the relatively bright primary contaminated the data on the secondary, which is a common effect for close visual binaries of similar brightnesses observed by HIPPARCOS such as HD 80606 / HD 80607.
- ^ The proper motions of HD 53680 are not corrected for the motion induced by its companion.
- ^ The parameters of HD 53706, in particular its luminosity, possess large errors due to the poor quality of the HIPPARCOS parallax.
- ^ The derived (not observed) parameters of HD 53680 A from Sahlmann et al. (2010) are unreliable, because they used a parallax 30.1 ± 0.6 mas of unclear source (The parallax from the original HIPPARCOS reduction is close to the current value, so the 30 mas value is likely a typographical error) which yields a somewhat high mass by about 0.1 M☉ and extremely high log g of 5.39 ± 0.29 cgs, a value similar to that of Proxima Centauri. The derived mass of HD 53680 B is therefore also somewhat higher than it should be.
References
edit- ^ a b c d e f g h i j k l m n o p q van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.
- ^ a b c d e f g h i j k l m Valenti, J. A.; Fischer, D. A. (2005). "Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs". The Astrophysical Journal Supplement Series. 159 (1): 141–166. Bibcode:2005ApJS..159..141V. doi:10.1086/430500.
- ^ a b c d e f g h i j k Sahlmann, J.; et al. (2010). "Search for brown-dwarf companions of stars". Astronomy & Astrophysics. 525: A95. arXiv:1009.5991. Bibcode:2011A&A...525A..95S. doi:10.1051/0004-6361/201015427. S2CID 119276951.
- ^ a b c d Houdebine, E. R. (September 2011). "Observation and modelling of main-sequence star chromospheres - XVI. Rotation of dK5 stars". Monthly Notices of the Royal Astronomical Society. 407 (3): 1657–1673. Bibcode:2011MNRAS.416.2233H. doi:10.1111/j.1365-2966.2011.19199.x.
- ^ a b c d e f g h Takeda, Genya; et al. (2007). "Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog". The Astrophysical Journal Supplement Series. 168 (2): 297–318. arXiv:astro-ph/0607235. Bibcode:2007ApJS..168..297T. doi:10.1086/509763. S2CID 18775378.
- ^ a b c "VizieR".
- ^ a b c d e Allen, C.; et al. (2000). "Wide binaries among high-velocity and metal-poor stars". Astronomy and Astrophysics. 356: 529. Bibcode:2000A&A...356..529A.
- ^ a b Makarov, V. V.; et al. (2005). "Statistical Constraints for Astrometric Binaries with Nonlinear Motion" (PDF). The Astronomical Journal. 129 (5): 2420–2427. Bibcode:2005AJ....129.2420M. doi:10.1086/429590. Archived from the original on September 24, 2017.
- ^ a b c Makarov, V. V.; et al. (2008). "Common Proper Motion Companions to Nearby Stars: Ages and Evolution". The Astrophysical Journal. 687 (1): 566–578. arXiv:0808.3414. Bibcode:2008ApJ...687..566M. doi:10.1086/591638. S2CID 17811620.
- ^ a b Endl, M.; et al. (2002). "The planet search program at the ESO Coudé Echelle spectrometer. III. The complete Long Camera survey results". Astronomy & Astrophysics. 392 (2): 671–690. arXiv:astro-ph/0207512. Bibcode:2002A&A...392..671E. doi:10.1051/0004-6361:20020937. S2CID 17393347.
- ^ a b Zechmeister, M.; et al. (2013). "The planet search programme at the ESO CES and HARPS. IV. The search for Jupiter analogues around solar-like stars". Astronomy & Astrophysics. 552: A78. arXiv:1211.7263. Bibcode:2012yCat..35520078Z. doi:10.1051/0004-6361/201116551. S2CID 53694238.
- ^ a b Udry, S. (2000). "The CORALIE Planet-Search Sample". From Extrasolar Planets to Cosmology: The VLT Opening Symposium. Eso Astrophysics Symposia. p. 571. Bibcode:2000fepc.conf..571U. doi:10.1007/10720961_83. ISBN 978-3-540-67163-3.
- ^ a b Jones, Hugh R. A.; et al. (2002). "Extrasolar planets around HD 196050, HD 216437 and HD 160691". Monthly Notices of the Royal Astronomical Society. 337 (4): 1170–1178. arXiv:astro-ph/0206216. Bibcode:2002MNRAS.337.1170J. doi:10.1046/j.1365-8711.2002.05787.x. S2CID 119520409.
- ^ a b Wittenmyer, Robert A.; et al. (2011). "On the Frequency of Jupiter Analogs". The Astrophysical Journal. 727 (2): 102. arXiv:1011.4720. Bibcode:2011ApJ...727..102W. doi:10.1088/0004-637X/727/2/102. S2CID 56204861.