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	\| ra = {{RA\|22\|34\|42.153}}<ref name=GaiaDR3/>		\| ra = {{RA\|22\|34\|42.153}}<ref name=GaiaDR3/>
	\| dec = {{DEC\|−03\|35\|58.17}}<ref name=GaiaDR3/>		\| dec = {{DEC\|−03\|35\|58.17}}<ref name=GaiaDR3/>
	\| appmag_v = 9.23<ref name=Anderson_Francis_2012/>		\| appmag_v = 9.23<ref name=Anderson_Francis_2012/><br>Min I: 9.86<br>Min II: 9.59<ref name=Samus_et_al_2017/>
	}}		}}
	{{Starbox character		{{Starbox character
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	\| b-v = 0.601{{±\|0.037}}<ref name=Anderson_Francis_2012/>		\| b-v = 0.601{{±\|0.037}}<ref name=Anderson_Francis_2012/>
	\| u-b = 0.029<ref name=Saputra_2020/>		\| u-b = 0.029<ref name=Saputra_2020/>
	\| variable =		\| variable = ]<ref name=Samus_et_al_2017/>
	}}		}}
	{{Starbox astrometry		{{Starbox astrometry
	\| radial_v =		\| radial_v = −9.59{{±\|0.46}}<ref name=Ibanoǧlu_et_al_2008/>
	\| prop_mo_ra = 73.192		\| prop_mo_ra = 73.192
	\| prop_mo_dec = −21.545		\| prop_mo_dec = −21.545
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	{{Starbox end}}		{{Starbox end}}

	'''LL Aquarii''' is an ] star system in the ] ] of ], abbreviated LL Aqr. At peak brightness it has a combined ] of 9.23,<ref name=Anderson_Francis_2012/> which is too dim to be visible to the ]. Based on ] measurements, it is located at a distance of approximately 447 ]s from the ].<ref name=GaiaDR3/>		'''LL Aquarii''' is an ] star system in the ] ] of ], abbreviated LL Aqr. At peak brightness it has a combined ] of 9.23,<ref name=Anderson_Francis_2012/> which is too dim to be visible to the ]. Based on ] measurements, it is located at a distance of approximately 447 ]s from the ].<ref name=GaiaDR3/> The system is drifting closer with a heliocentric ] of about −10 km/s.<ref name=Ibanoǧlu_et_al_2008/>

	==Observations==		==Observations==
			]'' data.<ref name=MAST/> 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 ] eclipsing binary based on ] observations made with the ] space observatory. It was assigned the ] LL Aqr in 1999.<ref name=Kazarovets_et_al_1999/> This is a ] forming a double-lined ]. In 2004, a more extensive ] showed an eccentric orbit with a ] 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.<ref name=Otero_Dubovsky_2004/> The first ] were published in 2008, showing an ] of 0.3095 with a mass ratio of 0.86. ]s indicated the stars are near the mid point of their ] lifetimes.<ref name=Ibanoǧlu_et_al_2008/>		In 1996, this star was found to be an ] eclipsing binary based on ] observations made with the ] space observatory. It was assigned the ] LL Aqr in 1999.<ref name=Kazarovets_et_al_1999/> This is a ] forming a double-lined ]. In 2004, a more extensive ] showed an eccentric orbit with a ] 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.<ref name=Otero_Dubovsky_2004/> The first ] were published in 2008, showing an ] of 0.3095 with a mass ratio of 0.86. ]s indicated the stars are near the mid point of their ] lifetimes.<ref name=Ibanoǧlu_et_al_2008/>

	The more massive member of the system, the primary component, has a ] of F9 V,<ref name=Smolec_et_al_2016/> matching an ]. 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 ] at an ] of around 6,080 K. It is spinning with a ] of {{val\|3.5\|0.5\|u=km/s}}. The ], or abundance of elements with mass greater ~~the~~ helium, is very nearly Sun-like.<ref name=Smolec_et_al_2016/>		The more massive member of the system, the primary component, has a ] of F9 V,<ref name=Smolec_et_al_2016/> matching an ]. 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 ] at an ] of around 6,080 K. It is spinning with a ] of {{val\|3.5\|0.5\|u=km/s}}. The ], or abundance of elements with mass greater than helium, is very nearly Sun-like.<ref name=Smolec_et_al_2016/>

	The secondary component is considered a ], which means its properties are close to Sun-like. It is a ] with a class of G3 V.<ref name=Smolec_et_al_2016/> Neither member of the system shows signs of ], being slowly rotating and not ]. ] between the two stars is negligible;<ref name=Southworth_2013/> they have an orbital separation of 40.7 times the radius of the Sun.<ref name=Smolec_et_al_2016/>		The secondary component is considered a ], which means its properties are close to Sun-like. It is a ] with a class of G3 V.<ref name=Smolec_et_al_2016/> Neither member of the system shows signs of ], being slowly rotating and not ]. ] between the two stars is negligible;<ref name=Southworth_2013/> they have an orbital separation of 40.7 times the radius of the Sun.<ref name=Smolec_et_al_2016/>
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	\| access-date=2024-12-29		\| access-date=2024-12-29
	\| postscript=. \| mode = cs2 }}</ref>		\| postscript=. \| mode = cs2 }}</ref>

			<ref name=MAST>{{citation \| postscript=.
			\| title=MAST: Barbara A. Mikulski Archive for Space Telescopes
			\| url=https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html
			\| publisher=Space Telescope Science Institute \| access-date=29 December 2024}}</ref>

	<ref name=GaiaDR3>{{Cite Gaia DR3 \| 2628040117046777984}}</ref>		<ref name=GaiaDR3>{{Cite Gaia DR3 \| 2628040117046777984}}</ref>
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	\| volume=1523 \| issue=1 \| at=id. 012021 \| date=April 2020		\| volume=1523 \| issue=1 \| at=id. 012021 \| date=April 2020
	\| doi=10.1088/1742-6596/1523/1/012021		\| doi=10.1088/1742-6596/1523/1/012021
	\| bibcode=2020JPhCS1523a2021S }}</ref>		\| bibcode=2020JPhCS1523a2021S \| doi-access=free
			}}</ref>

	<ref name=Smolec_et_al_2016>{{citation \| postscript=.		<ref name=Smolec_et_al_2016>{{citation \| postscript=.
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	\| last1=Otero \| first1=Sebastian A. \| last2=Dubovsky \| first2=Pavol A.		\| last1=Otero \| first1=Sebastian A. \| last2=Dubovsky \| first2=Pavol A.
	\| journal=Information Bulletin on Variable Stars		\| journal=Information Bulletin on Variable Stars
	\| volume=5557 \| page=1 \| ~~year~~=August 2004		\| volume=5557 \| page=1 \| date=August 2004
	\| bibcode=2004IBVS.5557....1O }}</ref>		\| bibcode=2004IBVS.5557....1O }}</ref>

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	\| volume=390 \| issue=3 \| pages=958–968 \| date=November 2008		\| volume=390 \| issue=3 \| pages=958–968 \| date=November 2008
	\| doi=10.1111/j.1365-2966.2008.13585.x		\| doi=10.1111/j.1365-2966.2008.13585.x
			\| doi-access=free
	\| bibcode=2008MNRAS.390..958I }}</ref>		\| bibcode=2008MNRAS.390..958I }}</ref>

	<ref name=Southworth_2013>{{citation \| postscript=.		<ref name=Southworth_2013>{{citation \| postscript=.
	\| title=The solar-type eclipsing binary system ~~LL Aquarii~~*		\| title=The solar-type eclipsing binary system LL Aquarii*
	\| first=J. \| last=Southworth		\| first=J. \| last=Southworth
	\| journal=Astronomy & Astrophysics		\| journal=Astronomy & Astrophysics
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	\| doi=10.1051/0004-6361/201322195 \| arxiv=1308.1320		\| doi=10.1051/0004-6361/201322195 \| arxiv=1308.1320
	\| bibcode=2013A&A...557A.119S }}</ref>		\| bibcode=2013A&A...557A.119S }}</ref>

			<ref name=Samus_et_al_2017>{{citation
			\| display-authors=1 \| last1=Samus \| first1=N. N.
			\| last2=Kazarovets \| first2=E. V. \| last3=Durlevich \| first3=O. V.
			\| last4=Kireeva \| first4=N. N. \| last5=Pastukhova \| first5=E. N.
			\| title=General Catalogue of Variable Stars
			\| version=5.1 \| journal=]
			\| year=2017 \| volume=61 \| issue=1 \| pages=80–88
			\| bibcode=2017ARep...61...80S \| doi=10.1134/S1063772917010085
			\| s2cid=125853869 \| postscript=. }}</ref>

	}}		}}

Latest revision as of 06:25, 6 January 2025

Binary star in the constellation Aquarius

LL Aquarii
Observation data Epoch J2000.0 Equinox J2000.0
Constellation	Aquarius
Right ascension	22 34 42.153
Declination	−03° 35′ 58.17″
Apparent magnitude (V)	9.23 Min I: 9.86 Min II: 9.59
Characteristics
Evolutionary stage	main sequence
Spectral type	F9 V + G3 V
U−B color index	0.029
B−V color index	0.601±0.037
Variable type	Algol
Astrometry

Radial velocity (R_v)	−9.59±0.46 km/s
Proper motion (μ)	RA: 73.192 mas/yr Dec.: −21.545 mas/yr
Parallax (π)	7.297 ± 0.0219 mas
Distance	447 ± 1 ly (137.0 ± 0.4 pc)
Absolute magnitude (M_V)	3.95

Orbit
Period (P)	20.178321(3) d
Semi-major axis (a)	40.744(7) `R`_☉
Eccentricity (e)	0.31654(7)
Inclination (i)	89.548(26)°
Longitude of the node (Ω)	32.11(14)°
Periastron epoch (T)	2,455,100.56106(79) JD
Argument of periastron (ω) (secondary)	155.50(4)°
Semi-amplitude (K₁) (primary)	49.948(13) km/s
Semi-amplitude (K₂) (secondary)	57.736(14) km/s
Details
Primary
Mass	1.1949(7) `M`_☉
Radius	1.321(6) `R`_☉
Luminosity	2.15(7) `L`_☉
Surface gravity (log g)	4.274(4) cgs
Temperature	6,080(45) K
Metallicity	0.02(4) dex
Rotational velocity (v sin i)	3.5(5) km/s
Secondary
Mass	1.0337(7) `M`_☉
Radius	1.002(5) `R`_☉
Luminosity	0.958(35) `L`_☉
Surface gravity (log g)	4.451(4) cgs
Temperature	5,703(50) K
Metallicity	0.03(6) dex
Rotational velocity (v sin i)	3.6(4) km/s
Other designations
LL Aqr, BD−04° 5706, HD 213896, HIP 111454, SAO 146171, PPM 206522
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, 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. The system is drifting closer with a heliocentric radial velocity of about −10 km/s.

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.

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. 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. 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.

The more massive member of the system, the primary component, has a stellar classification of F9 V, 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.

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. 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; they have an orbital separation of 40.7 times the radius of the Sun.

References

^ 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.
^ 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.
^ 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.
^ 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.
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.
^ 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.
"LL Aqr", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2024-12-29.
MAST: Barbara A. Mikulski Archive for Space Telescopes, Space Telescope Science Institute, retrieved 29 December 2024.
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.
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.
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.

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