R Aqr

Constellation
Aquarius

Equatorial coordinates
α = 23 43 49.493
δ = -15 17 04.663

Galactic coordinates
l = 66.5168°
b = -70.3256°

Suspected	1921^Ref
Confirmed	1921^Ref
Symbiotic IR type	S^Ref
Hot component type	accreting-only^Ref
Outbursts	Yes^Ref

Identifiers

R Aqr	IRAS 23412-1533	GSC2.4.2 SB7J000082	AAVSO 000-BCR-898
SIMBAD V* R Aqr	Pan-STARRS 89653559562708874	SAO 165849	VSX 846
GAIA DR3 2419576358847950592	SkyMapper 234349.49-151704.9	WRAY -	GCVS R Aqr
2MASS J23434939-1517043	HIP 117054	Hen -	BD -16 6352
WISE J234349.53-151704.8	TYC 6404-77-1	ESO -	HD 222800

Symbiotic Catalogs

Bidelman (1954)	-	Allen (1984)	R Aqr (Conf.)	Belzcyński et al. (2001)	R Aqr (Conf.)
Gaposchkin (1957)	R Aqr (Conf.)	Kenyon (1986)	R Aqr (Conf.)	Akras et al. (2019)	R Aqr (Conf.)
Boyarchuk (1969)	R Aqr (Conf.)	Vaidis (1988, 1991)	R Aqr (Conf.)

Position

Right ascension (°)	355.9562^Ref	Parallax (mas)	2.593±0.333^Ref	Reddening E(B-V) (mag)	0.02±0.0^Ref ^{, Note}
Declination (°)	-15.2846^Ref	Distance (kpc)	0.2^Ref, 0.18-0.30^Ref, 0.22±0.05^Ref, 0.2^Ref, 0.24^Ref, 0.28±0.015^Ref, 0.178±0.018^Ref 0.39^Ref ^{, Note} -^{, Note}
Galactic longitude (°)	66.5168^Ref	Proper motion in α (mas/yr)	26.88±0.23^Ref
Galactic latitude (°)	-70.3256^Ref	Proper motion in δ (mas/yr)	-30.41±0.18^Ref

Observations

X-Ray	Yes^Ref	IR type	S^Ref	Radio	Yes^Ref
X-Ray type	β/δ^Ref	J (mag)	-0.16^Ref	Flickering	No^Ref
GALEX FUV (mag)	-	H (mag)	-1.10^Ref	Outbursts	Yes^Ref
GALEX NUV (mag)	-	K (mag)	-1.61^Ref	Outburst type	-
IUE	Yes^Ref	WISE W1 (mag)	1.72^Ref	Jets	Yes^Ref
FUSE	No^Ref	WISE W2 (mag)	2.00^Ref	Resolved nebula	Yes^Ref
U (mag)	-	WISE W3 (mag)	-2.87^Ref	IPmax (eV)	97.1 (UV)^Ref, 35.1^Ref
B (mag)	10.92^Ref	WISE W4 (mag)	-3.20^Ref	[O III] lines	Yes^Ref
V (mag)	9.59^Ref	IRAS 12μm (Jy)	1580.00^Ref	He II lines	No^Ref
R (mag)	9.37^Ref	IRAS 25μm (Jy)	544.00^Ref	[Fe VII] lines	No^Ref
I (mag)	-	IRAS 60μm (Jy)	66.70^Ref	O VI lines	No^Ref
BP (mag)	10.76^Ref	IRAS 100μm (Jy)	16.60^Ref
G (mag)	6.71^Ref	AKARI S09 (Jy)	-
RP (mag)	4.87^Ref	AKARI S18 (Jy)	349.10^Ref

Orbit

Orbital period (days)	16070^Ref, 15943±471^Ref	γ velocity (km/h)	-28.4^Ref, -24.9±0.2^Ref	Size of giant’s orbit (AU)	5.9^Ref
Eccentricity	0.6^Ref, 0.25±0.07^Ref	RV of giant (km/h)	5^Ref, 4.0±0.4^Ref	Separation (AU)	14-18^Ref, 14.2-16.8^Ref
Inclination (°)	70^Ref	Inferior conj. of giant (JD)	-	Mass function	0.107^Ref, 0.096^Ref
Eclipses	Yes?^Ref			Mass ratio	1.2-2.1^Ref
Orbital ephemeris	-

Cool component

Spectral type	M7 III^Ref, M6.5-8.5 III^Ref, M7 III^Ref, M8 III^Ref	Mass (M_⊙)	1-2^Ref, 1.5^Ref, 1-1.5^Ref	Pulsation	Yes^Ref
Eff. temperature (K)	2800^Ref	Radius (R_⊙)	300^Ref	Type	Mira^Ref
IR type	S^Ref	Luminosity (L_⊙)	9000^Ref	Pulsation period (days)	387^Ref, 388.1±0.1^Ref
Metallicity [Fe/H]	-			Pulsation ephemeris	Max (V)= 2442404.2±0.4 + 388.1±0.1 x E^Ref

Hot component

Type/Spectral type	WD^Ref	Mass (M_⊙)	0.5-1^Ref, 0.57-1.02^Ref	Spin period (min)	-
Shell-burning/Accreting-only	accreting-only^Ref	Radius (R_⊙)	-	Accretion disk	-
Eff. temperature (K)	>50000^Ref, 50000-60000^Ref, 40000^Ref	Luminosity (L_⊙)	5-20^Ref, 10^Ref
Lower limit (K)	-
Upper limit (K)	-

Links

SIMBAD CDS Portal ARAS Database

Notes

In Merrill (1950), variability with a period of 26.7 years was reported, initially considered as orbital by Jacobsen & Wallerstein (1975). Subsequently, Kurochkin (1976) identified variability with a period of 24 years. In Willson et al. (1981), the system was claimed to exhibit eclipses with a period of 44 years. Considering the orbital period, Hinkle et al. (1989) suggested it must be either between 18 - 21 years or longer than 32 years. Different estimates emerged in subsequent studies, with McIntosh & Rustan (2007) proposing an orbital period of 34.6 +- 1.2 years, and Gromadzki & Mikołajewska (2009) determining an orbital period of 43.6 years. The detection of the [Fe XIII] line in the spectrum of R Aqr was reported by Zirin (1976). In Burgarella et al. (1992), it was claimed that two major outbursts occurred before 190 and 650 years. Furthermore, Yang et al. (2005) suggested that outbursts of R Aqr were detected by Korean astronomers in 1073/1074 (see also Tanabe & Motizuki, 2012). In Nichols et al. (2007), variability with a period of 1734 seconds in hard X-ray data was detected. The binary system was resolved using SPHERE/ZIMPOL data by Schmid et al. (2017).

References

Bujarrabal, V., Agúndez, M., Gómez-Garrido, M. et al., 2021, A&A, 651, A4, 2021A&A...651A...4B
Bujarrabal, V., Alcolea, J., Mikołajewska, J. et al., 2018, A&A, 616, L3, 2018A&A...616L...3B
Burgarella, D., Vogel, M., Paresce, F., 1992, A&A, 262, 83, 1992A&A...262...83B
Gromadzki, M., Mikołajewska, J., 2009, A&A, 495, 3, 931, 2009A&A...495..931G
Hinkle, K. H., Wilson, T. D., Scharlach, W. W. G. et al., 1989, AJ, 98, 1820, 1989AJ.....98.1820H
Hollis, J. M., Kafatos, M., Michalitsianos, A. G. et al., 1985, ApJ, 289, 765, 1985ApJ...289..765H
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Kafatos, M., Michalitsianos, A. G., Hollis, J. M., 1986, ApJS, 62, 853, 1986ApJS...62..853K
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