HD 41742 and HD 41700
  | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Puppis |
| HD 41742 A | |
| Right ascension | 06h 04m 40.101s[1] |
| Declination | −45° 04′ 44.10″[1] |
| Apparent magnitude (V) | 5.975±0.009[2] |
| HD 41742 B | |
| Right ascension | 06h 04m 39.782s[3] |
| Declination | −45° 04′ 48.78″[3] |
| Apparent magnitude (V) | 8.867±0.028[2] |
| HD 41700 (C) | |
| Right ascension | 06h 04m 28.439s[4] |
| Declination | −45° 02′ 11.77″[4] |
| Apparent magnitude (V) | 6.343±0.010[2] |
| Characteristics | |
| HD 41742 A | |
| Spectral type | F6V[5]/K-MV(MS) |
| B−V color index | 0.493±0.009[6] |
| HD 41742 B | |
| Spectral type | K3V[5] |
| B−V color index | 1.014±0.076[2] |
| HD 41700 (C) | |
| Spectral type | F7.5V[5] |
| B−V color index | 0.517±0.005[6] |
| Astrometry | |
| HD 41742 A | |
| Radial velocity (Rv) | 27.0±2.5[7][note 1] km/s |
| Proper motion (μ) | RA: −80.831[1] mas/yr Dec.: +251.617[1] mas/yr |
| Parallax (π) | 35.779 ± 0.2768 mas[1] |
| Distance | 91.2 ± 0.7 ly (27.9 ± 0.2 pc) |
| Absolute magnitude (MV) | 3.853±0.024[8] |
| HD 41742 B | |
| Proper motion (μ) | RA: −84.025[3] mas/yr Dec.: 237.521[3] mas/yr |
| Parallax (π) | 37.0030 ± 0.0525 mas[3] |
| Distance | 88.1 ± 0.1 ly (27.02 ± 0.04 pc) |
| Absolute magnitude (MV) | 6.745±0.043[8] |
| HD 41700 (C) | |
| Radial velocity (Rv) | 27.4±0.4[7] km/s |
| Proper motion (μ) | RA: −82.262[4] mas/yr Dec.: 246.246[4] mas/yr |
| Parallax (π) | 36.8531 ± 0.0162 mas[4] |
| Distance | 88.50 ± 0.04 ly (27.13 ± 0.01 pc) |
| Absolute magnitude (MV) | 4.221±0.025[8] |
| Details | |
| HD 41742 A | |
| Mass | 1.20+0.07 −0.06[7] M☉ / ~≥0.21 ± 0.06 M☉ |
| Radius | 1.4[1] R☉ |
| Luminosity | 2.7[1] L☉ |
| Surface gravity (log g) | 4.30 ± ~0.10[7] cgs |
| Temperature | 6,363±85[7] K |
| Metallicity [Fe/H] | −0.17±0.10[7] dex |
| Rotation | ≤2.0 days (maximum rotational period, derived from v sin i if i = 90°)[9] |
| Rotational velocity (v sin i) | 26.7±1.3[9] km/s |
| Age | 3.3[1] Gyr |
| HD 41742 B | |
| Mass | 0.80[10] M☉ |
| Radius | 0.93[3] R☉ |
| Luminosity | 0.25[3] L☉ |
| Surface gravity (log g) | 4.38[3] cgs |
| Temperature | 4,294[3] K |
| Metallicity [Fe/H] | −0.22[3] dex |
| HD 41700 (C) | |
| Mass | 1.13+0.04 −0.07[7] M☉ |
| Radius | 1.2[4] R☉ |
| Luminosity | 1.8[4] L☉ |
| Surface gravity (log g) | 4.36[7] cgs |
| Temperature | 6,165±80[7] K |
| Metallicity [Fe/H] | −0.19±0.10[7] dex |
| Rotational velocity (v sin i) | 16.6±1.0[11] km/s |
| Age | 3.7[4] Gyr |
| Other designations | |
| HD 41742 A: HIP 28790, TYC 8101-1755-1, HR 2158 | |
| HD 41742 B: TYC 8101-1757-1 | |
| HD 41700 (C): HIP 28764, GJ 9200, TYC 8101-309-1, HR 2157 | |
| Database references | |
| HD 41742 A | |
| SIMBAD | data |
| HD 41742 B | |
| SIMBAD | data |
| HD 41700 (C) | |
| SIMBAD | data |
HD 41742 and HD 41700 is a star system that lies approximately 88 light-years away in the constellation of Puppis. The system consists of two bright stars where the primary is orbited by two fainter stars, making it a quadruple with an unequal hierarchy.
Component discovery
[edit]
HD 41742 B was discovered early on in the history of visual binaries, due to the brightness of the primary. The earliest measurement in the Washington Double Star Catalog (WDS) dates to 1837 and was made by William Herschel, stating a position angle of 246° and a separation of 1.1" for the companion.[12] Surprisingly, recent measures suggest that the secondary has moved significantly over the two centuries since, with it lying at a position angle of around 215° and a separation increasing between 5.30" in the late 1970s[13] to 5.95" in 2010.[14] This translates to a minimum change in physical separation between 142 and 159 AU over 35 years,[10] which suggests that HD 41742 B is moving quickly away from the primary.
Lying at a considerably wider separation, HD 41700 was first observed relative to HD 41742 later than the tighter binary, despite being much brighter. The first measurement in the WDS dates to 1854 and was again made by Herschel, giving a position angle of 320° and a separation of 174".[12] More recent values agree on the position angle, but suggest a separation closer to 200". The wide separation of this tertiary component means that it has a separate Hipparcos entry to the primary, which confirms that the two stars lie at the same distance and are co-moving. The physical separation between the two is about 0.026 parsecs (0.084 light-years), or approximately 17200 AU.[15] This is comparable to the ~15000 AU separation between Alpha Centauri AB and Proxima Centauri; such wide separations between components are relatively rare, at least for solar-type stars.
Radial velocity observations of HD 41742 A with the HARPS spectrograph detected variations on a level of several km/s over a period of months, indicating that the star is a single-lined spectroscopic binary (SB1).[16] Though an orbital fit was not attempted, A good orbital fit is possible (left), which implies that HD 41742 Ab has a minimum mass of ~0.2 M☉, and is on a high eccentricity ~222-day orbit around the 1.2 M☉ primary. Given that the lines of the secondary are not detected, it must have a significantly lower luminosity than the primary, indicating that it is of late spectral type.
Properties
[edit]
On the celestial sphere, HD 41742/41700 can be seen as a 6th magnitude star (a magnitude barely observable by the naked eye under good conditions) lying close to the border between Puppis and Pictor. The nearest bright star to its location is the 4th magnitude Eta Columbae approximately two arcminutes to the north; The system lies about a quarter of the distance between Eta Columbae and Canopus (Alpha Carinae) on the sky.
HD 41742 A and HD 41700 (C) are similar stars, with their colours indicating spectral types of F6 and F7.5; this means that the two stars are about 500 K hotter than the Sun, and in turn the difference in temperature between the stars is about 150 kelvins.[5] The stars lie slightly below the main sequence on the Hertzsprung–Russell diagram (left image), which is probably due to their sub-solar metallicity (Fe/H ≈ −0.2).[7]
HD 41742 B is a much cooler star than the brighter components; its B-V indicates a spectral type of K3, making it approximately 1000 K cooler than the Sun.[5] It lies on the main sequence on the HRD (left image), and its photometry is fully consistent with an 0.8 M☉ dwarf.[10]
Indication of a young age for the HD 41742/41700 system was first found Henry et al. (1996), detecting large chromospheric activity in HD 41700; they measured a log R'HK of −4.35 for the star,[17] significantly higher than a "quiet" value of < −4.70, indicating that the system is considerably younger than 1 Gyr. The brightest stars in the system are both moderately fast rotators for late-F dwarfs, again indicating that they are young.[9][11] Finally, HD 41700 has a somewhat large lithium content; because lithium is used up by a star at an approximately constant rate over its lifetime, this can be used to estimate a star's age. For HD 41700, its lithium abundance indicates an age of 200 ± 50 million years.[11]
Some young star systems remain loosely associated with other stars that formed in the same molecular cloud as they move through space, known as a moving group. The HD 41742/41700 system has space velocities of (UVW) = −37.8, −10.4, −14.6 km/s,[18] which is similar to those of the Hyades (UVW = −39.7, −17.7, −2.4 km/s[18]); however, the system is probably not a Hyad because it has a lower peculiar velocity than expected,[18] as well as a lower metallicity and lithium age than the Hyades.
Another feature prevalent around young stars are debris disks. For HD 41742 A and HD 41700 (C), IRAS and ISO detected infra-red excesses,[19][20] which are typically indicative of disks of material re-radiating absorbed light at redder wavelengths; however, in both cases evidence against the excesses have been found. For HD 41742 A, the excess is offset by 26",[21] which is large enough so that contamination from another object is likely responsible for the excess, while for HD 41700 (C) the excess has not been confirmed by Spitzer observations.[22]
Planet searches
[edit]HD 41700 (C) is included on the CORALIE and Keck-HIRES planet search samples.[23][24][25] No variability has been announced so far, so the star likely does not host a close-in, easily detectable giant planet.
HD 41742 A was included on a planet search around early-type (<~F7) stars with HARPS that detected its spectroscopic binarity,[16] as discussed above.
Notes
[edit]- ^ Value not accounting for binary orbit
References
[edit]- ^ a b c d e f g h i Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d e Høg, E.; et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27. Bibcode:2000A&A...355L..27H.
- ^ a b c d e f g h i j k Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d e f g h i Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d e f A Modern Mean Stellar Color and Effective Temperatures (Teff) # Sequence for O9V-Y0V Dwarf Stars, E. Mamajek, 2011, website
- ^ a b c 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 Casagrande, L.; et al. (2011). "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey". Astronomy. 530: A138. arXiv:1103.4651. Bibcode:2011A&A...530A.138C. doi:10.1051/0004-6361/201016276. S2CID 56118016.
- ^ a b c d The relevant calculation for absolute magnitude is , where is the apparent magnitude and is the distance in light-years.
- ^ a b c d Ammler-von Eiff, Matthias; Reiners, Ansgar (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics, 542: A116, arXiv:1204.2459, Bibcode:2012A&A...542A.116A, doi:10.1051/0004-6361/201118724, S2CID 53666672.
- ^ a b c d Ehrenreich, D.; et al. (2010). "Deep infrared imaging of close companions to austral A- and F-type stars". Astronomy. 523: A73. arXiv:1007.0002. Bibcode:2010A&A...523A..73E. doi:10.1051/0004-6361/201014763. S2CID 54913363.
- ^ a b c d Weise, P.; et al. (2010). "Rotational velocities of nearby young stars". Astronomy and Astrophysics. 517: A88. arXiv:1005.0984. Bibcode:2010A&A...517A..88W. doi:10.1051/0004-6361/201014453. S2CID 119267923.
- ^ a b c Mason; et al. "WDS 06047-4505". The Washington Visual Double Star Catalog. Retrieved 2013-08-02.
- ^ a b van Albada-van Dien, E. (1985). "Photographic observations of visual double stars". Astronomy and Astrophysics Supplement Series. 60: 315. Bibcode:1985A&AS...60..315V.
- ^ a b Tokovinin, Andrei; et al. (2010). "Subsystems in Nearby Solar-type Wide Binaries". The Astronomical Journal. 140 (2): 510–517. arXiv:1006.1253. Bibcode:2010AJ....140..510T. doi:10.1088/0004-6256/140/2/510. S2CID 73629363.
- ^ a b Shaya, Ed J.; Olling, Rob P. (January 2011), "Very Wide Binaries and Other Comoving Stellar Companions: A Bayesian Analysis of the Hipparcos Catalogue", The Astrophysical Journal Supplement, 192 (1): 2, arXiv:1007.0425, Bibcode:2011ApJS..192....2S, doi:10.1088/0067-0049/192/1/2, S2CID 119226823
- ^ a b c Lagrange, A. -M.; et al. (2009). "Extrasolar planets and brown dwarfs around A-F type stars. VI. High precision RV survey of early type dwarfs with HARPS". Astronomy and Astrophysics. 495 (1): 335–352. arXiv:0809.4636. Bibcode:2009A&A...495..335L. doi:10.1051/0004-6361:200810105. S2CID 62894956.
- ^ a b Henry, Todd J.; et al. (1996). "LA Survey of Ca II H and K Chromospheric Emission in Southern Solar-Type Stars". The Astronomical Journal. 111: 439. Bibcode:1996AJ....111..439H. doi:10.1086/117796.
- ^ a b c d Montes, D.; et al. (2001). "Late-type members of young stellar kinematic groups - I. Single stars". Monthly Notices of the Royal Astronomical Society. 328 (1): 45–63. arXiv:astro-ph/0106537. Bibcode:2001MNRAS.328...45M. doi:10.1046/j.1365-8711.2001.04781.x. S2CID 55727428.
- ^ a b Mannings, Vincent; Barlow, Michael J. (1998). "Candidate Main-Sequence Stars with Debris Disks: A New Sample of Vega-like Sources". The Astrophysical Journal. 497 (1): 330–341. Bibcode:1998ApJ...497..330M. CiteSeerX 10.1.1.502.7594. doi:10.1086/305432. S2CID 122421281.
- ^ a b Decin, G.; et al. (2000). "The Vega phenomenon around G dwarfs". Astronomy and Astrophysics. 357: 533. Bibcode:2000A&A...357..533D.
- ^ a b Sylvester, Roger J.; et al. (2000). "Optical, infrared and millimetre-wave properties of Vega-like systems - IV. Observations of a new sample of candidate Vega-like sources". Monthly Notices of the Royal Astronomical Society. 313 (1): 73–86. Bibcode:2000MNRAS.313...73S. doi:10.1046/j.1365-8711.2000.03194.x.
- ^ a b Hillenbrand, Lynne A.; et al. (2008). "The Complete Census of 70 μm-bright Debris Disks within "the Formation and Evolution of Planetary Systems" Spitzer Legacy Survey of Sun-like Stars". The Astrophysical Journal. 677 (1): 630–656. arXiv:0801.0163. Bibcode:2008ApJ...677..630H. doi:10.1086/529027. S2CID 17641245.
- ^ a b Mortier, A.; et al. (2013). "On the functional form of the metallicity-giant planet correlation". Astronomy. 551: A112. arXiv:1302.1851. Bibcode:2013A&A...551A.112M. doi:10.1051/0004-6361/201220707. S2CID 56350455.
- ^ a b Wright, J. T.; et al. (2004). "Chromospheric Ca II Emission in Nearby F, G, K, and M Stars". The Astrophysical Journal Supplement Series. 152 (2): 261–295. arXiv:astro-ph/0402582. Bibcode:2004ApJS..152..261W. doi:10.1086/386283. S2CID 16257628.
- ^ a b Isaacson, Howard; Fischer, Debra (2010). "Chromospheric Activity and Jitter Measurements for 2630 Stars on the California Planet Search". The Astrophysical Journal. 725 (1): 875–885. arXiv:1009.2301. Bibcode:2010ApJ...725..875I. doi:10.1088/0004-637X/725/1/875. S2CID 118577960.
