HD 1976: Difference between revisions

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	{{Starbox catalog		{{Starbox catalog
	\|names={{odlist\|2MASS=J00241564+5201119\|AG=+51°39\|BD=+51°62\|ALS=14565\|GC=476\|GSC=03260-02342\|HD=1976\|HIP=1921\|HR=91\|PPM=25297\|SAO=21366\|TIC=202418751\|TYC=3260-2342-1\|Gaia DR3=418916648901801728\|WDS=J00243+5201AB\|V=V746 Cassiopeiae}},<ref name="SIMBAD"/>		\|names={{odlist\|2MASS=J00241564+5201119\|AG=+51°39\|BD=+51°62\|ALS=14565\|GC=476\|GSC=03260-02342\|HD=1976\|HIP=1921\|HR=91\|PPM=25297\|SAO=21366\|TIC=202418751\|TYC=3260-2342-1\|Gaia DR3=418916648901801728\|WDS=J00243+5201AB\|V=V746 Cassiopeiae}}<ref name="SIMBAD"/>
	}}		}}
	{{Starbox reference		{{Starbox reference
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	{{Starbox end}}		{{Starbox end}}
	'''HD 1976''' is a ] in the deep northern ] of ], ~~approximately~~ {{convert\|1100\|ly\|pc\|abbr=off}} from ]. It has the ] '''V746 Cassiopeiae''' (abbreviated to V746 Cas). The system is faintly visible to the naked eye under dark skies, having an ] of 5.580. It consists of an inner pair between a ] ] and a less massive unknown-type star, which is distantly orbited by another B-type subgiant. It is currently moving closer towards the ] at a heliocentric ] of −9.70 km/s.		'''HD 1976''' is a ] in the deep northern ] of ], somewhere around {{convert\|1100\|ly\|pc\|abbr=off}} from ]. It has the ] '''V746 Cassiopeiae''' (abbreviated to V746 Cas). The system is faintly visible to the naked eye under dark skies, having an ] of 5.580. It consists of an inner pair between a ] ] and a less massive unknown-type star, which is distantly orbited by another B-type subgiant. It is currently moving closer towards the ] at a heliocentric ] of −9.70 km/s.

			==Measurement discrepancies==
⚫	==Stellar ~~properties~~==
			Several measurements have been made on the distance to the star system, namely {{val\|406\|54\|ul=pc}},<ref name=EDR3/> {{val\|307\|59\|u=pc}},<ref name=vanLeeuwen2007/> and {{val\|186\|24\|u=pc}},<ref name=Gardner2022/> but all of them have large ]s and differ substantially from one another. The first two agree within the wide ]s, while the third value is thought to be too low due to the noisy ] orbit swaying the ]. In a 2022 study, the total mass of the inner pair could only be constrained poorly at {{val\|9\|5}} {{Solar mass\|link=y}} because of this uncertainty, and the masses of the individual stars were estimated from a mass ratio of {{val\|1.57\|0.28}} and an adopted{{efn\|From Kervella et al. 2019.<ref name=Kervella2019/>}} mass figure of 6.348 {{Solar mass}}.<ref name=Gardner2022/>
	* uncertain distance

			Stellar parameter estimates via ] also yield different results depending on whether the spectral data near the ] H-β, H-γ, and H-δ is used in calculations, which are often affected by instrumental problems and rectification systematics.<ref name=Harmanec2017/>
		⚫	==Stellar components==
	===HD 1976 Aa===		===HD 1976 Aa===
	* large discrepancy		* large discrepancy
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	<ref name=TYC2000>{{cite journal \| display-authors=1 \| title=The Tycho-2 Catalogue of the 2.5 Million Brightest Stars \| last1=Høg \| first1=E. \| last2=Fabricius \| first2=C. \| last3=Makarov \| first3=V. V. \| last4=Urban \| first4=S. \| last5=Corbin \| first5=T. \| last6=Wycoff \| first6=G. \| last7=Bastian \| first7=U. \| last8=Schwekendiek \| first8=P. \| last9=Wicenec \| first9=A. \| journal=Astronomy and Astrophysics \| volume=355 \| issue=1 \| pages=L27–L30 \| date=February 2000 \| bibcode=2000A&A...355L..27H}}</ref>		<ref name=TYC2000>{{cite journal \| display-authors=1 \| title=The Tycho-2 Catalogue of the 2.5 Million Brightest Stars \| last1=Høg \| first1=E. \| last2=Fabricius \| first2=C. \| last3=Makarov \| first3=V. V. \| last4=Urban \| first4=S. \| last5=Corbin \| first5=T. \| last6=Wycoff \| first6=G. \| last7=Bastian \| first7=U. \| last8=Schwekendiek \| first8=P. \| last9=Wicenec \| first9=A. \| journal=Astronomy and Astrophysics \| volume=355 \| issue=1 \| pages=L27–L30 \| date=February 2000 \| bibcode=2000A&A...355L..27H}}</ref>

	<ref name=Gardner2022>{{Cite journal \| display-authors=3 \|doi-access=free\|last=Gardner \|first=Tyler \|last2=Monnier \|first2=John D. \|last3=Fekel \|first3=Francis C. \|last4=Le Bouquin \|first4=Jean-Baptiste \|last5=Scovera \|first5=Adam \|last6=Schaefer \|first6=Gail \|last7=Kraus \|first7=Stefan \|last8=Adams \|first8=Fred C. \|last9=Anugu \|first9=Narsireddy \|last10=Berger \|first10=Jean-Philippe \|last11=Ten Brummelaar \|first11=Theo \|last12=Davies \|first12=Claire L. \|last13=Ennis \|first13=Jacob \|last14=Gies \|first14=Douglas R. \|last15=Johnson \|first15=Keith J. C. \|date=2022-11-01 \|title=ARMADA. II. Further Detections of Inner Companions to Intermediate-mass Binaries with Microarcsecond Astrometry at CHARA and VLTI \|url=https://iopscience.iop.org/article/10.3847/1538-3881/ac8eae \|journal=The Astronomical Journal \|volume=164 \|issue=5 \|pages=184 \|doi=10.3847/1538-3881/ac8eae \|issn=0004-6256}}</ref>		<ref name=Gardner2022>{{Cite journal \| display-authors=3 \|doi-access=free\|last=Gardner \|first=Tyler \|last2=Monnier \|first2=John D. \|last3=Fekel \|first3=Francis C. \|last4=Le Bouquin \|first4=Jean-Baptiste \|last5=Scovera \|first5=Adam \|last6=Schaefer \|first6=Gail \|last7=Kraus \|first7=Stefan \|last8=Adams \|first8=Fred C. \|last9=Anugu \|first9=Narsireddy \|last10=Berger \|first10=Jean-Philippe \|last11=Ten Brummelaar \|first11=Theo \|last12=Davies \|first12=Claire L. \|last13=Ennis \|first13=Jacob \|last14=Gies \|first14=Douglas R. \|last15=Johnson \|first15=Keith J. C. \|date=2022-11-01 \|title=ARMADA. II. Further Detections of Inner Companions to Intermediate-mass Binaries with Microarcsecond Astrometry at CHARA and VLTI \|url=https://iopscience.iop.org/article/10.3847/1538-3881/ac8eae \|journal=The Astronomical Journal \|volume=164 \|issue=5 \|pages=184 \|doi=10.3847/1538-3881/ac8eae \|issn=0004-6256}}{{Creative Commons text attribution notice\|cc=by4\|from this source=yes}}</ref>

	<ref name=Harmanec2017>{{cite journal \| display-authors=3 \| last=Harmanec \| first=P. \| last2=Brož \| first2=M. \| last3=Mayer \| first3=P. \| last4=Zasche \| first4=P. \| last5=Kotková \| first5=L. \| last6=Nemravová \| first6=J. A. \| last7=Dukes \| first7=R. J. \| last8=Korčáková \| first8=D. \| last9=Šlechta \| first9=M. \| last10=Kıran \| first10=E. \| last11=Kříček \| first11=R. \| last12=Juryšek \| first12=J. \| title=Improved model of the triple system V746 Cassiopeiae that has a bipolar magnetic field associated with the tertiary \| journal=Astronomy & Astrophysics \| publisher=EDP Sciences \| volume=609 \| date=2017-12-22 \| issn=0004-6361 \| doi=10.1051/0004-6361/201628363 \| doi-access=free \| page=A5}}</ref>		<ref name=Harmanec2017>{{cite journal \| display-authors=3 \| last=Harmanec \| first=P. \| last2=Brož \| first2=M. \| last3=Mayer \| first3=P. \| last4=Zasche \| first4=P. \| last5=Kotková \| first5=L. \| last6=Nemravová \| first6=J. A. \| last7=Dukes \| first7=R. J. \| last8=Korčáková \| first8=D. \| last9=Šlechta \| first9=M. \| last10=Kıran \| first10=E. \| last11=Kříček \| first11=R. \| last12=Juryšek \| first12=J. \| title=Improved model of the triple system V746 Cassiopeiae that has a bipolar magnetic field associated with the tertiary \| journal=Astronomy & Astrophysics \| publisher=EDP Sciences \| volume=609 \| date=2017-12-22 \| issn=0004-6361 \| doi=10.1051/0004-6361/201628363 \| doi-access=free \| page=A5}}</ref>
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	<ref name=Mamajek2022>{{cite web\|last=Mamajek\|first=Eric\|title=A Modern Mean Dwarf Stellar Color and Effective Temperature Sequence\|url=http://www.pas.rochester.edu/~emamajek/EEM_dwarf_UBVIJHK_colors_Teff.txt\|date=2022-04-16\|access-date=2024-11-11}}</ref>		<ref name=Mamajek2022>{{cite web\|last=Mamajek\|first=Eric\|title=A Modern Mean Dwarf Stellar Color and Effective Temperature Sequence\|url=http://www.pas.rochester.edu/~emamajek/EEM_dwarf_UBVIJHK_colors_Teff.txt\|date=2022-04-16\|access-date=2024-11-11}}</ref>

			<ref name=vanLeeuwen2007>{{cite journal \| last=van Leeuwen \| first=F. \| title=Validation of the new Hipparcos reduction \| journal=Astronomy & Astrophysics \| volume=474 \| issue=2 \| date=2007 \| issn=0004-6361 \| doi=10.1051/0004-6361:20078357 \| doi-access=free \| pages=653–664}}</ref>

			<ref name=Kervella2019>{{cite journal \| last=Kervella \| first=Pierre \| last2=Arenou \| first2=Frédéric \| last3=Mignard \| first3=François \| last4=Thévenin \| first4=Frédéric \| title=Stellar and substellar companions of nearby stars from Gaia DR2: Binarity from proper motion anomaly \| journal=Astronomy & Astrophysics \| volume=623 \| date=2019 \| issn=0004-6361 \| doi=10.1051/0004-6361/201834371 \| doi-access=free \| page=A72}}</ref>
	}}		}}
	* {{cite journal \| last=Docobo \| first=J. A. \| last2=Costa \| first2=J. M. \| title=First orbits for the visual double stars ADS 328, ADS 9043, and ADS 13048 \| journal=The Astrophysical Journal Supplement Series \| publisher=American Astronomical Society \| volume=60 \| year=1986 \| issn=0067-0049 \| doi=10.1086/191106 \| page=945}}		* {{cite journal \| last=Docobo \| first=J. A. \| last2=Costa \| first2=J. M. \| title=First orbits for the visual double stars ADS 328, ADS 9043, and ADS 13048 \| journal=The Astrophysical Journal Supplement Series \| publisher=American Astronomical Society \| volume=60 \| year=1986 \| issn=0067-0049 \| doi=10.1086/191106 \| page=945}}

Revision as of 10:26, 13 November 2024

Triple star system in the constellation Cassiopeia

HD 1976
Observation data Epoch J2000 Equinox J2000
Location of HD 1976 (circled)
Constellation	Cassiopeia
Right ascension	00 24 15.65400
Declination	+52° 01′ 11.7032″
Apparent magnitude (V)	5.580 (combined)
Characteristics
Spectral type	(B5IV + unknown) + ~B5-6IV
U−B color index	-0.619
B−V color index	-0.121
J−H color index	-0.102
J−K color index	-0.106
Variable type	Slowly pulsating B-type star (A; disputed)
Astrometry

Radial velocity (R_v)	−9.70 ± 0.49 km/s
Proper motion (μ)	RA: 15.504 mas/yr Dec.: -4.061 mas/yr
Parallax (π)	2.4621 ± 0.33 mas
Distance	approx. 1,300 ly (approx. 410 pc)

Orbit
Primary	HD 1976 Aa
Companion	HD 1976 Ab
Period (P)	25.4163±0.0008 d
Semi-major axis (a)	0.42±0.05 mas
Eccentricity (e)	0.05±0.03
Inclination (i)	100.7±1.2°
Longitude of the node (Ω)	339.9±1.1°
Periastron epoch (T)	59477±5
Argument of periastron (ω) (secondary)	61±52°
Orbit
Primary	HD 1976 A
Companion	HD 1976 B
Period (P)	171±3 yr
Semi-major axis (a)	208.0±2.7 mas
Eccentricity (e)	0.162±0.008
Inclination (i)	62.8±0.4°
Longitude of the node (Ω)	27.8±0.4°
Periastron epoch (T)	33710±679
Argument of periastron (ω) (secondary)	306.0±4°
Details
HD 1976 Aa
Mass	4.71+0.17 −0.16, 6.45±0.17, 6.348 `M`_☉
Radius	5.74+0.18 −0.16, 5.24+0.14 −0.10 `R`_☉
Surface gravity (log g)	3.59±0.01, 3.81±0.01 cgs
Temperature	15534±69, 16526+100 −82 K
Rotational velocity (v sin i)	178±6, 170±4 km/s
Age	~60 Myr
HD 1976 Ab
Mass	1.31, 1.87, 4.0±0.7 `M`_☉
Radius	1.40, 1.82 `R`_☉
Surface gravity (log g)	4.27, 4.18 cgs
Temperature	6385+565 −657, 8071+266 −352 K
Rotational velocity (v sin i)	165 km/s

HD 1976 B
Mass	2.65±0.25, 6.10+0.27 −0.26 `M`_☉
Radius	3.40+0.29 −0.26, 4.48±0.20 `R`_☉
Surface gravity (log g)	3.80±0.03. 3.92±0.02 cgs
Temperature	14750±66, 13620+154 −144 K
Rotational velocity (v sin i)	63+9 −8, 73+6 −5 km/s

Other designations
V746 Cassiopeiae, AG+51°39, BD+51°62, Gaia DR3 418916648901801728, GC 476, HD 1976, HIP 1921, HR 91, SAO 21366, PPM 25297, WDS J00243+5201AB, TIC 202418751, TYC 3260-2342-1, GSC 03260-02342, 2MASS J00241564+5201119
Database references
SIMBAD	HD 1976

HD 1976 is a hierarchical triple system in the deep northern constellation of Cassiopeia, somewhere around 1,100 light-years (340 parsecs) from Earth. It has the variable-star designation V746 Cassiopeiae (abbreviated to V746 Cas). The system is faintly visible to the naked eye under dark skies, having an apparent magnitude of 5.580. It consists of an inner pair between a B-type subgiant and a less massive unknown-type star, which is distantly orbited by another B-type subgiant. It is currently moving closer towards the Solar System at a heliocentric radial velocity of −9.70 km/s.

Measurement discrepancies

Several measurements have been made on the distance to the star system, namely 406±54 pc, 307±59 pc, and 186±24 pc, but all of them have large errors and differ substantially from one another. The first two agree within the wide error bars, while the third value is thought to be too low due to the noisy radial velocity orbit swaying the semi-amplitude. In a 2022 study, the total mass of the inner pair could only be constrained poorly at 9±5 M_☉ because of this uncertainty, and the masses of the individual stars were estimated from a mass ratio of 1.57±0.28 and an adopted mass figure of 6.348 M_☉.

Stellar parameter estimates via astronomical spectroscopy also yield different results depending on whether the spectral data near the Balmer lines H-β, H-γ, and H-δ is used in calculations, which are often affected by instrumental problems and rectification systematics.

Stellar components

HD 1976 Aa

large discrepancy
pulsations
magnetism

HD 1976 Ab

The only component whose spectrum cannot be directly observed, HD 1976 Ab is in a nearly circular (eccentricity 0.05) 25-day orbit with Aa.

As is the case with the other two stars, its physical properties are very uncertain. A 2017 study presented two sets of possible characteristics, each corresponding to an A-type (1.87 M_☉) and F-type main-sequence star (1.31 M_☉). In 2022, however, a far higher mass of 4.0±0.7 M_☉ was reported, which resembles that of a late B-type main-sequence star.

HD 1976 B

magnetism

Footnotes

From Kervella et al. 2019.
In comparison, a typical B7V star has a mass of about 3.92 M_☉.

References

^ Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
^ Høg, E.; et al. (February 2000). "The Tycho-2 Catalogue of the 2.5 Million Brightest Stars". Astronomy and Astrophysics. 355 (1): L27 – L30. Bibcode:2000A&A...355L..27H.
^ Neiner, C.; Tkachenko, A.; MiMeS collaboration (2014). "Discovery of a magnetic field in the B pulsating system HD 1976". Astronomy & Astrophysics. 563. EDP Sciences: L7. doi:10.1051/0004-6361/201423595. ISSN 0004-6361.
^ Harmanec, P.; Brož, M.; Mayer, P.; et al. (22 December 2017). "Improved model of the triple system V746 Cassiopeiae that has a bipolar magnetic field associated with the tertiary". Astronomy & Astrophysics. 609. EDP Sciences: A5. doi:10.1051/0004-6361/201628363. ISSN 0004-6361.
^ "HD 1976". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 10 November 2024.
^ Gardner, Tyler; Monnier, John D.; Fekel, Francis C.; et al. (1 November 2022). "ARMADA. II. Further Detections of Inner Companions to Intermediate-mass Binaries with Microarcsecond Astrometry at CHARA and VLTI". The Astronomical Journal. 164 (5): 184. doi:10.3847/1538-3881/ac8eae. ISSN 0004-6256. This article incorporates text from this source, which is available under the CC BY 4.0 license.
van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy & Astrophysics. 474 (2): 653–664. doi:10.1051/0004-6361:20078357. ISSN 0004-6361.
Kervella, Pierre; Arenou, Frédéric; Mignard, François; Thévenin, Frédéric (2019). "Stellar and substellar companions of nearby stars from Gaia DR2: Binarity from proper motion anomaly". Astronomy & Astrophysics. 623: A72. doi:10.1051/0004-6361/201834371. ISSN 0004-6361.
Mamajek, Eric (16 April 2022). "A Modern Mean Dwarf Stellar Color and Effective Temperature Sequence". Retrieved 11 November 2024.

Docobo, J. A.; Costa, J. M. (1986). "First orbits for the visual double stars ADS 328, ADS 9043, and ADS 13048". The Astrophysical Journal Supplement Series. 60. American Astronomical Society: 945. doi:10.1086/191106. ISSN 0067-0049.

Variable stars

Pulsating

Cepheids and cepheid-like	Type I (Classical cepheids, Delta Scuti) Type II (BL Herculis, W Virginis, RV Tauri) RR Lyrae Rapidly oscillating Ap SX Phoenicis
Blue-white with early spectra	Alpha Cygni Beta Cephei Slowly pulsating B-type PV Telescopii Blue large-amplitude pulsator
Long-period	Mira Semiregular Slow irregular
Other	Gamma Doradus Solar-like oscillations White dwarf

Eruptive

Protostar and PMS	Herbig Ae/Be Orion FU Orionis T Tauri
Giants and supergiants	Luminous blue variable R Coronae Borealis (DY Persei) Yellow hypergiant
Eruptive binary	Double periodic FS Canis Majoris RS Canum Venaticorum
Other	Flare Gamma Cassiopeiae Lambda Eridani Wolf–Rayet

Cataclysmic

Rotating

Non-spherical	Rotating ellipsoidal
Stellar spots	BY Draconis FK Comae Berenices
Magnetic fields	α Canum Venaticorum Pulsar SX Arietis

Eclipsing

Star portal * List

Constellation of Cassiopeia

Stars

Bayer	α (Schedar) β (Caph) γ (Navi/Tsih) δ (Ruchbah) ε (Segin) ζ (Fulu) η (Achird) θ (Marfak) ι κ λ μ ν ξ ο π ρ σ τ υ υ (Castula) φ χ ψ ω
Flamsteed	1 2 4 6 9 10 12 42 47 48 (A) 49 50 54
Variable	R S TZ WZ YZ (21) AO AR PZ V373 V509 V547 V669 V705 V762 V863 V773 V987 V1022 V1405
HR	5 91 144 196 244 273 297 743 932 8832 8853 8881
HD	861 7924 7977 15558 17156 (Nushagak) 240210 240237 240429 240430
Other	BD+60°2522 Gliese 49 IRAS 23304+6147 LS I +61 303 PSR J0205+6449 Tycho G 4U 0142+61 WR 2 WR 3

Exoplanets	HD 7924 b HD 17156 b HD 219134 b c d e (h) f g HD 240210 b HD 240237 b

Star clusters	Messier 52 Messier 103 NGC 103 NGC 110 NGC 129 NGC 133 NGC 136 NGC 146 NGC 189 NGC 225 NGC 358 NGC 366 NGC 381 NGC 433 NGC 436 NGC 457 NGC 559 NGC 637 NGC 654 NGC 659 NGC 663 NGC 1027 NGC 7789 NGC 7790 Trumpler 3

Nebulae

NGC	281 7635
Other	3C 58 Cassiopeia A Heart Nebula IC 289 IC 1805 KjPn 8 LBN 114.55+00.22 Sh 2-185 Westerhout 5

Galaxies

NGC	147 185 278
Other	Andromeda VII 3C 20 3C 35 Dwingeloo 1 Dwingeloo 2 MB 3 IC 10 Maffei 1 Maffei 2 QSO B0153+744

Astronomical events	SN 1181 SN 1572 (B)

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