LL Aquarii

Last updated
LL Aquarii
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Aquarius [1]
Right ascension 22h 34m 42.153s [2]
Declination −03° 35′ 58.17″ [2]
Apparent magnitude  (V)9.23 [1]
Min I: 9.86
Min II: 9.59 [3]
Characteristics
Evolutionary stage main sequence [4]
Spectral type F9 V + G3 V [5]
U−B color index 0.029 [6]
B−V color index 0.601±0.037 [1]
Variable type Algol [3]
Astrometry
Radial velocity (Rv)−9.59±0.46 [7] km/s
Proper motion (μ)RA: 73.192 mas/yr [2]
Dec.: −21.545 mas/yr [2]
Parallax (π)7.297±0.0219  mas [2]
Distance 447 ± 1  ly
(137.0 ± 0.4  pc)
Absolute magnitude  (MV)3.95 [1]
Orbit [4]
Period (P)20.178322(1) days
Semi-major axis (a)40.744±0.007  R☉ [5]
Eccentricity (e)0.3163±0.0003
Inclination (i)89.545±0.003°
Longitude of the node (Ω)32.11±0.14 [5] °
Periastron epoch (T)2460223.84444(1)  BJD
Argument of periastron (ω)
(secondary)		155.69±0.12°
Semi-amplitude (K1)
(primary)		49.948±0.013 [5]  km/s
Semi-amplitude (K2)
(secondary)		57.736±0.014 [5]  km/s
Details [4]
Primary
Mass 1.1947(9)  M☉
Radius 1.3180(13)  R☉
Luminosity 2.377  L☉
Surface gravity (log g)4.2755(9)  cgs
Temperature 6,242±50  K
Metallicity [Fe/H]0.075±0.030  dex
Rotation 19.1±3.2 days
Rotational velocity (v sin i)3.5±0.5 [5]  km/s
Age 3.01±0.12  Gyr
Secondary
Mass 1.0334(6)  M☉
Radius 0.9927(8)  R☉
Luminosity1.030  L☉
Surface gravity (log g)4.4587(8)  cgs
Temperature 5,839±44  K
Metallicity [Fe/H]0.052±0.027  dex
Rotation 14.0±1.7 days
Rotational velocity (v sin i)3.6±0.4 [5]  km/s
Age 2.67±0.12  Gyr
Other designations
LL Aqr, BD−04°5706, HD 213896, HIP 111454, SAO 146171, PPM 206522 [8]
Database references
SIMBAD data

LL Aquarii is an eclipsing binary star system in the equatorial constellation of Aquarius, abbreviated LL Aqr. At peak brightness it has a combined apparent visual magnitude of 9.23, [1] which is too dim to be visible to the naked eye. Based on parallax measurements, it is located at a distance of approximately 447  light years from the Sun. [2] The system is drifting closer with a heliocentric radial velocity of about −10 km/s. [7]

Contents

Observations

A light curve for LL Aquarii, plotted from TESS data. The main plot shows the complete light curve, and the inset plot shows that primary (red) and secondary (green) minima with an expanded horizontal scale. LLAqrLightCurve.png
A light curve for LL Aquarii, plotted from TESS data. The main plot shows the complete light curve, and the inset plot shows that primary (red) and secondary (green) minima with an expanded horizontal scale.

In 1996, this star was found to be an Algol-type eclipsing binary based on photometric observations made with the Hipparcos space observatory. It was assigned the variable-star designation LL Aqr in 1999. [10] This is a detached system forming a double-lined spectroscopic binary. In 2004, a more extensive light curve showed an eccentric orbit with a period of 20.1784 days. During the primary eclipse, the system dropped to magnitude 9.86, while the secondary eclipse showed a magnitude of 9.59. [11] The first orbital elements were published in 2008, showing an orbital eccentricity of 0.3095 with a mass ratio of 0.86. Stellar models indicated the stars are near the mid point of their main sequence lifetimes. [7]

The more massive member of the system, the primary component, has a stellar classification of F9 V, [5] matching an F-type main-sequence star. It has 19.5% more mass than the Sun and a 32% greater girth. This star is radiating 2.15 times the luminosity of the Sun from its photosphere at an effective temperature of around 6,080 K. It is spinning with a projected rotational velocity of 3.5±0.5 km/s. The metallicity, or abundance of elements with mass greater than helium, is very nearly Sun-like. [5]

The secondary component is considered a solar twin, which means its properties are close to Sun-like. It is a G-type main-sequence star with a class of G3 V. [5] Neither member of the system shows signs of stellar activity, being slowly rotating and not emitting X-rays. Tidal effects between the two stars is negligible; [12] they have an orbital separation of 40.7 times the radius of the Sun. [5]

References

  1. 1 2 3 4 5 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv: 1108.4971 , Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID   119257644.
  2. 1 2 3 4 5 6 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.
  3. 1 2 Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports , 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID   125853869.
  4. 1 2 3 Miller, N. J.; Maxted, P. F. L.; Hahlin, A.; Graczyk, D. (2025-11-20), "Fundamental effective temperature measurements for eclipsing binary stars - VII. The solar twin in LL Aquarii", Monthly Notices of the Royal Astronomical Society , arXiv: 2511.16519 , doi: 10.1093/mnras/staf2078 .
  5. 1 2 3 4 5 6 7 8 9 10 11 Graczyk, D.; et al. (October 2016), "A solar twin in the eclipsing binary LL Aquarii", Astronomy & Astrophysics, 594, id. A92, arXiv: 1608.01000 , Bibcode:2016A&A...594A..92G, doi:10.1051/0004-6361/201628918.
  6. ↑ Saputra, M. B. (April 2020), "Atmospheric model and synthetic spectrum of LL Aquarii using Kurucz model", Journal of Physics: Conference Series, 1523 (1), id. 012021, Bibcode:2020JPhCS1523a2021S, doi: 10.1088/1742-6596/1523/1/012021 .
  7. 1 2 3 Ibanoǧlu, C.; et al. (November 2008), "Spectroscopic and photometric observations of the selected Algol-type binaries - III. LL Aquarii, MP Delphini and NSV 20913", Monthly Notices of the Royal Astronomical Society, 390 (3): 958–968, Bibcode:2008MNRAS.390..958I, doi: 10.1111/j.1365-2966.2008.13585.x .
  8. ↑ "LL Aqr", SIMBAD , Centre de données astronomiques de Strasbourg , retrieved 2024-12-29.
  9. ↑ MAST: Barbara A. Mikulski Archive for Space Telescopes, Space Telescope Science Institute, retrieved 29 December 2024.
  10. ↑ Kazarovets, E. V.; et al. (1999), "The 74th Special Name-list of Variable Stars", Information Bulletin on Variable Stars, 4659: 1, Bibcode:1999IBVS.4659....1K.
  11. ↑ Otero, Sebastian A.; Dubovsky, Pavol A. (August 2004), "New Elements for 80 Eclipsing Binaries IV", Information Bulletin on Variable Stars, 5557: 1, Bibcode:2004IBVS.5557....1O.
  12. ↑ Southworth, J. (September 2013), "The solar-type eclipsing binary system LL Aquarii*", Astronomy & Astrophysics, 557: 557, arXiv: 1308.1320 , Bibcode:2013A&A...557A.119S, doi:10.1051/0004-6361/201322195, A119.

Further reading

This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.