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Chapter 17
Cataclysmic and Symbiotic Variables
W.M. Sparks, S.G. Starrfield,
E.M. Sion, S.N. Shore,
G. Chanmugam†, and R.F. Webbink
17.1
17.1
Types of Cataclysmic Variables . . . . . . . . . . . . . 429
17.2
Types of Symbiotic Variables . . . . . . . . . . . . . . 447
TYPES OF CATACLYSMIC VARIABLES
A cataclysmic variable (CV) [1, 2] is a binary star system in which a white dwarf primary accretes
hydrogen-rich material usually through an accretion disk from a Roche lobe filling secondary that is on
or near the main sequence. The CVs consist of several classes such as classical novae, recurrent novae,
nova-likes, dwarf novae, helium CVs, and magnetic CVs. The distributions of their orbital periods are
shown in Figure 17.1. Catalogues of CVs are found in [3, 4]. Proceedings of CV conferences [5–9] are
bountiful sources of information.
A classical nova [10–12] is a CV that has undergone an outburst (9–15 mag. increase) which
ejects a shell of gas at high velocity. Tables 17.1 and 17.2 contain the brightest and best-observed
classical novae in our Galaxy. More extensive lists are found in [13] and [3]. Table 17.3 lists the
brightest novae from 1991 to 1995. Well-observed novae in the Large Magellanic Cloud are given in
Table 17.4. Classical novae are commonly assumed to be caused by a thermonuclear runaway in the
accreted material on the white dwarf. The classical novae are also designated as CNO and ONeMg
novae according to the composition of the ejecta (see Table 17.5). It is inferred that these novae occur
on CO and ONeMg white dwarfs, respectively, and their ejecta include white dwarf material. As their
name implies, recurrent novae have been observed to undergo more than one outburst. Although there
are currently only nine members listed in this class (see Tables 17.6 and 17.7), it may be necessary
to subdivide them according to their type of outburst or their type of secondary when they are better
understood. In some systems the outbursts are probably caused by thermonuclear runaways, but in
† Deceased.
429
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430 / 17
C ATACLYSMIC AND S YMBIOTIC VARIABLES
Figure 17.1. The orbital period distributions of the cataclysmic variables.
other systems the outburst may result from an episodic mass transfer accompanied by the release of
gravitational energy onto the primary which could be a white dwarf or a main-sequence star [14, 15].
In addition, for some recurrent novae, the secondary is a late-type giant.
The dwarf novae (Table 17.8) [16] undergo a periodic brightening (2–5 mag.) on a time scale of
weeks to years with little or no mass ejection aside from the wind outflow during the outburst in most of
the systems. Most dwarf novae change from having an emission line spectrum to having an absorption
line spectrum during outburst. This phenomenon is normally assumed to be caused by an instability in
the accretion disk surrounding the white dwarf. The SU UMa stars are a subclass of dwarf novae that
also show semiperiodic outbursts of unusually large amplitude (superoutburst), distinguished by the
appearance at outburst maximum of periodic modulations (superhumps) in the light curve with periods
a few percent larger than the orbital period. Dwarf novae that show occasional standstills (episodes of
intermediate brightness lasting days to years) during decline from maximum are termed Z Cam stars.
The remainder of the dwarf novae are called U Gem systems after the original prototype.
The nova-likes [16] are CVs that have the appearance of quiescent classical novae, i.e., they are
probably classical novae that have not had a recorded outburst. Table 17.9 contains the best observed
nova-likes. Additional listings are found in Ritter [3]. There are two subclasses of nova-likes: UX UMa
and VY Scl. The UX UMa systems look like dwarf novae in a permanent outburst state while the
VY Scl systems (or antidwarf novae) are normally in a high state but have slow, short excursions to a
low state. These variations of luminosity are probably due to changes in the accretion rate. The helium
CVs (or AM CVn systems) are transferring helium-rich material instead of hydrogen-rich material.
Otherwise they appear to be nova-likes.
The white dwarf in a magnetic CV has a sufficiently strong magnetic field to channel the flow of
accreting material at least near the white dwarf’s surface [17]. The magnetic CVs may be divided into
two subclasses depending on whether the white dwarf is rotating synchronously (Table 17.10) with
its binary companion, as in the AM Her binaries or polars, or asynchronously (Table 17.11) as in the
DQ Her binaries or intermediate polars. In the AM Her binaries, the magnetic field is sufficiently strong
so that the accretion flows via an accretion column and no accretion disk is formed. In the DQ Her
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17.1 T YPES OF C ATACLYSMIC VARIABLES / 431
binaries, the magnetic field is probably weaker and an accretion disk may form but is disrupted close
to the white dwarf’s surface.
Being a member of one class of CVs does not prevent a system from being a member of another.
For example, GK Per, an old classical nova, also shows dwarf nova outbursts. Nova V1500 Cyg is also
an AM Her system. The space density of CVs, ρcv , is a subject of much controversy. Assuming that
the novae, dwarf novae, and nova-likes found in a galactic plane survey [18] represent all the CVs, their
space density, ρcv , is (5.3–8.2)×10−7 pc−3 . However, if novae fade considerably between outbursts,
then a higher space density like that of ρcv ≥ 3 × 10−5 pc−3 found in a deep but narrow survey [19]
may be more realistic.
Many of the following tables make use of the SIMBAD database, operated at CDS (Centre de
Donnees Stellaires), Strasbourg, France. Uncertain numbers are followed by a colon.
Table 17.1. Selected list of classical novae.
Name
(alternate name)
α a (2000)
hr min sec
δ a (2000)
deg min sec
b (deg)
bb (deg)
GK Per
(N Per 1901)
T Aur
(N Aur 1891)
RR Pic
(N Pic 1925)
CP Pup
(N Pup 1942)
GQ Mus
(N Mus 1983)
DQ Her
(N Her 1934)
FH Ser
(N Ser 1970)
V693 CrA
(N CrA 1981)
V603 Aql
(N Aql 1918)
V1370 Aql
(N Aql 1982)
PW Vul
(N Vul 1984 No. 1)
HR Del
(N Del 1967)
V1500 Cyg
(N Cyg 1975)
V1668 Cyg
(N Cyg 1978)
OS And
(N And 1986)
03 31 11.82
43 54 16.8
150.55
−10.60
05 31 59.06
30 26 45.2
176.79
−2.30
06 35 36.05
−62 38 23.4
272.30
−25.71
08 11 45.96
−35 21 05.7
252.59
−1.08
11 52 02.35
−67 12 20.2
296.92
−4.78
18 07 30.17
45 51 31.9
73.09
26.68
18 30 46.92
02 36 51.5
32.59
6.33
18 41 57.63
−37 31 13.1
357.51
18 48 54.50
00 35 02.9
32.82
1.37
19 23 21.10
02 29 26.1
38.43
−5.43
19 26 05.03
27 21 58.3
60.80
5.55
20 42 20.18
19 09 40.3
62.96
−13.64
21 11 36.61
48 09 01.9
89.48
−0.00
21 42 35.22
44 01 54.9
90.42
−6.70
23 12 05.76
47 28 19.7
105.69
−11.97
−13.79
m cmax
m cmin
t3d
(days)
Light
curve
Refs.
Secondary
spectral
typee
0.2v
13.0v
4.1B
14.9B
1.2v
12.3v
0.2v
15.0v
7.2v
17.5v
1.3v
14.7v
4.4v
16.1v
6.5v
> 19v
−1.4v
11.6v
7.5p
20.0p
6.4v
17.0v
3.3v
12.1v
2.0B
16.3B
6.0v
20:
6.2v
17.8v
13
[1]
K2 IV–V
[2]
100
[3]
150
[4, 5]
8
[4, 6]
45
[8]
94
[4, 9]
62
[11]
12
[12]
8
[4, 13]
13:
[14, 15]
97
[16]
230
[17]
3.6
[19, 20]
23
[21, 22]
22
[23]
> M6
[7]
M3 V
[10]
K8
[18]
Notes
a Adapted from Duerbeck [24] and precessed to equinox 2000.
b Galactic coordinates.
c Maximum and minimum magnitudes from Warner [25]. and the light curve references B, v, and p are the blue, visual, and
photographic magnitudes.
d The time for the visual light curve to fall three magnitudes after maximum, t , was taken from Duerbeck [24].
3
e The secondary spectral types are from spectroscopic or infrared photometric observations and do not include estimates
from mass determinations.
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432 / 17
C ATACLYSMIC AND S YMBIOTIC VARIABLES
References
1. Sabbadin, F., & Bianchini, A. 1983, A&AS, 54, 393
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3. Leavitt, H.S. 1920, Harvard Annuals, 84, 121
4. Payne-Gaposchkin, C. 1957, The Galactic Novae (North-Holland, Amsterdam)
5. Spencer Jones, H. 1931, Cape Obs. Ann., 10, part 9
6. Pettit, E. 1954, PASP, 66, 142
7. Szkody, P., & Feinswog, L. 1988, ApJ, 334, 422
8. Krautter, J. et al. 1984, A&A, 137, 307
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10. Young, P., & Schneider, D.P. 1981, ApJ, 247, 960
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13. Campbell, L. 1919, Harvard Annuals, 81, 113
14. Rosino, L., Iijima, T., & Ortolani, S. 1983, MNRAS, 205, 1069
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Table 17.2. Data for selected classical novae.
Name
E(B − V )a
Nebular
shell
studiesb
Distancec
(pc)
Max.
abs.
mag.
GK Per
T Aur
RR Pic
CP Pup
0.3 [1]
0.6 [9]
0.07 [16]
0.08 [23]
[2]
[9, 10]
[17]
[23]
490n
1300n
460n
835n
−9.2n
−8.4n
−7.3n
−9.7n
GQ Mus
0.45 [28]
4280
−7.4
DQ Her
0.11 [31]
560n
−7.8n
FH Ser
0.4 [42]
850n
V693 CrA
0.56 [44]
V603 Aql
0.07 [16]
V1370 Aql
0.6 [52]
PW Vul
0.45 [54]
HR Del
0.29 [58]
V1500 Cyg
0.5 [66]
[10, 32]
[10, 46]
Periodd
(days)
Rapid optical
oscillation
periode (s)
Expansion
velocity
(km/s)
Outburst
spectra. f
Quiescent
spectra. f
Descriptiong
[8]
[15]
[22]
[24]
VF
MF
S
VF
1.996 803 [3]
0.204 378 29 [11]
0.145 025 5 [18]
0.061 43 [24]
0.068 34 [25]
0.059 4 [29]
∼ 350 QPO [4]
1200 [5]
[12]
655 [13]
20–40 QPO [19] 475 [13]
710 [13]
[6, 7]
[14]
[20, 21]
[26, 27]
800 [28]
[28, 30]
0.193 620 6
[33, 34, 35]
71.074 514
[36, 37]
384 [38]
[39, 40]
[41]
−6.5n
560 [13]
[43]
[43]
5030
−8.8
2200 [44]
[44, 45]
370n
−9.5n
1700 [5]
[50]
2800 [53]
[52, 53]
285 [56]
[57]
520 [13]
1180 [13]
0.138 15 [47]
0.144 854 [48, 49]
2050
−6.6
0.2137 [55]
[59, 60]
850n
−7.3n
[67]
1080n
−9.8n
0.214 165 [61]
0.1775 [62]
0.139 613 [68, 69]
[12]
[51]
MF
CNO
no dust
MF
CNO
dust
MF
C dust
VF
ONeMg
VF
[58, 63]
[64, 65]
VF
ONeMg
C, SiC,
SiO2
dust
MF
Solar
C dust
VS
[70, 71]
[68]
VF
CNO
Sp.-V/AQuan/1999/10/28:17:09
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17.1 T YPES OF C ATACLYSMIC VARIABLES / 433
Table 17.2. (Continued.)
Nebular
shell
studiesb
Distancec
(pc)
Max.
abs.
mag.
Periodd
(days)
0.1384 [73]
Name
E(B − V )a
V1668 Cyg
0.4 [72]
3660
−8.1
OS And
0.25 [76]
7200
−8.2
Rapid optical
oscillation
periode (s)
Expansion
velocity
(km/s)
Outburst
spectra. f
760 [72]
[74, 75]
1000 [77]
[78]
Quiescent
spectra. f
Descriptiong
F
CNO
C dust
F
CNO
Notes
a The color excess, E(B − V ), is assumed to be related to the visual interstellar extinction, A , by A = 3.2E(B − V ).
v
v
b In addition to these nebular shell studies, a short spectroscopic description of the nova remnant is given by Duerbeck and
Seitter [79].
c The distances and absolute maximum magnitudes that are followed by an “n” have been determined by the nebular
expansion parallax method. The angular shell sizes are from Cohen and Rosenthal [13], except for V1500 Cyg [80], DQ
Her [38], and FH Ser [42]. The other distances and absolute magnitudes are found from the maximum magnitude −t2
relationship derived by Cohen [80] and assuming t2 ∼ t3/2 [81]. The time for the visual light curve to fall after maximum by
n magnitudes is denoted by tn .
d The spectroscopic period is the first entry while the photometric period is the second if it is different. Orbital parameters
can usually be found in the reference for the spectroscopic period.
e If only a reference is given in this column, it means an unsuccessful search.
f Only optical references are given. Surveys or catalogues of novae exist in the radio [82, 83], infrared [84–86], visual [87,
88], ultraviolet [89, 90], and X-ray [91–93] spectral regions. References of observations for individual novae can be found in
Payne-Gaposchkin [94], Ritter [95–97], Duerbeck [98], and Bode et al. [99]. Finding charts can be found in these last two
references and in Williams [87].
g The speed class is defined by Payne-Gaposchkin [94] as
Speed class
Rate of decline
(mag./day)
Very fast (VF)
Fast (F)
Moderately fast (MF)
Slow (S)
Very slow (VS)
> 0.20
0.18 to 0.08
0.07 to 0.025
0.024 to 0.013
0.013 to 0.008
The type of nova is defined by the strong enhancement above solar values of the chemical composition of the ejecta (CNO
or ONeMg) and often implies the composition of the white dwarf. The types of dust formed, if any, is quoted from Gehrz [56].
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Williams, G. 1983, ApJS, 53, 523
Bruch, A. 1984, A&AS, 56, 441
Friedjung, M. 1989, in Classical Novae, edited by by M.F. Bode and A. Evans (Wiley, New York), p. 187
Starrfield, S., & Snijders, M.A.J. 1987, in Scientific Accomplishments of the IUE Satellite, edited by Y. Kondo (Reidel,
Dordrecht), p. 377
Becker, R.H. 1989, in Classical Novae, edited by M.F. Bode and A. Evans (Wiley, New York), p. 215
Córdova, F.A., & Mason, K.O. 1983, in Accretion-driven Stellar X-ray Sources, edited by W.H.G. Lewin and E.P.J. van
den Heuvel (Cambridge University Press, Cambridge), p. 147
Eracleous, M., Halpern, J., & Patterson, J. 1991, ApJ, 382, 290
Payne-Gaposchkin, C. 1957, The Galactic Novae (North-Holland, Amsterdam)
Ritter, H. 1984, A&AS, 57, 385
Ritter, H. 1987, A&AS, 70, 335
Ritter, H. 1990, A&AS, 85, 1179
Duerbeck, H.W. 1987, A Reference Catalogue and Atlas of Galactic Novae (Reidel, Dordrecht); Space Sci. Rev., 45,
Nos. 1–2
Bode, M.F., Duerbeck, H.W., & Evans, A. 1989, in Classical Novae, edited by M.F. Bode and A. Evans (Wiley, New York),
p. 249
Table 17.3. Recent novae.
Name
(alternate
name)
α (2000)
hr min sec
δ (2000)
deg min sec
Date of
discovery
IAU
Circ.
No.
m max
t3 a
(days)
E(B − V )b
FWHMc
emission vel.
(km/s)
V351 Pup
(N Pup 91)
8 11 38.38
−35 07 30.4
27 Dec 1991
5422
6.4v
3000
V4160 Sgr
(N Sgr 91)
V838 Her
(N Her 91)
18 14 13.83
−32 12 28.5
29 July 1991
5313
7v
8000
18 46 31.48
+12 14 01.8
24 Mar 1991
5222
5.3v
2.8
0.6
6000
V1974 Cyg
(N Cyg 92)
20 30 31.66
+52 37 50.8
20 Feb 1992
5454
4.9B
43
0.35 ± 0.05
2000
V705 Cas
(N Cas 93)
V1425 Aql
(N Aql 95)
23 41 47.25
+57 30 59.7
7 Dec 1993
5902
5.3v
19 05 26.64
−01 42 03.3
7 Feb 1995
6133
6.2:v
22:
≥ 0.56
1600
Notes
a The time for the visual light curve to fall three magnitudes after maximum.
b The color excess.
c The full width half maximum velocity of the emission lines in IUE spectra measured by S. Shore.
d The description is the same as in Table 17.2 for classical novae.
Desc.d
ONeMg
no dust
VF
ONeMg
ONeMg
Dust
VF
ONeMg
No dust
MF
CO
Dust
ONeMg
Dust
F
Sp.-V/AQuan/1999/10/28:17:09
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436 / 17
C ATACLYSMIC AND S YMBIOTIC VARIABLES
Table 17.4. Recent novae in the Large Magellanic Cloud [1, 2].
Nova
α (2000)
hr min sec
δ (2000)
deg min sec
IAU Circ. No.
LMC V3479
LMC V1161
LMC V2361
LMC V1341
LMC V0850
LMC 1992
LMC 1995
5 35 29.33
5 08 01.10
5 23 21.82
5 09 58.40
5 03 44.99
5 19 19.84
5 26 50.33
−70 21 29.4
−68 37 37.7
−69 29 48.5
−71 39 51.6
−70 18 13.7
−68 54 35.1
−70 01 23.8
4569
4663
4946
4964
5244
5651
6143
Outburst
Vmax
Type
Remarks
21 Mar 1988
12 Oct 1988
16 Jan 1990
15 Feb 1990
18 Apr 1991
11 Nov 1992
2 Mar 1995
11.0
10.4
10.6
11.9
8.9
10.2
11.3
Dust, CNO
ONeMg
ONeMg
Recurrent
CNO?
CNO
CNO
a
b
c
d
e
f
Notes
a UV versus optical analysis: Austin, S., Starrfield, S., Saizar, P., Shore, S.N., & Sonneborn, G. 1990, in Evolution in
Astrophysics: IUE in the Era of New Space Missions, edited by E. Rolfs (ESA SP 310), p. 367. Possible dust-forming
nova.
b UV description: IAU Circ. No. 4669. First extragalactic ONeMg nova.
c t (optical) = 5.8 days. Sonneborn, G., Shore, S.N., & Starrfield, S.G. 1990, in Evolution in Astrophysics: IUE in
3
the Era of New Space Missions, edited by E. Rolfs (ESA SP 310), p. 439; see also, Starrfield, S., Shore, S.N., Sparks,
W.M., Sonneborn, G., Truran, J.W., & Politano, M. 1992, ApJ, 391, L71.
d Recurrence of Nova LMC 1968. Dynamics, abundances: Shore, S.N., Starrfield, S., Sonneborn, G., Williams,
R.E., Haumy, M., Cassatella, A., & Drechsel, H. 1991, ApJ, 370, 193. First spectroscopically confirmed, extragalactic
recurrent nova; U Sco analog (low mass companion, helium rich).
eF
−10 erg s−1 cm−2 ; t (UV) = 140 days; delay: optical versus UV peak ≈ 10 days. This was
UV,max = 1.64 × 10
3
the intrinsically brightest nova yet observed in the Local Group. Probable CNO nova.
f Star is a match to the Galactic nova OS And 1986.
References
1. General reference for LMC novae: van den Bergh, S. 1988, PASP, 100, 1486.
2. General reference for M31 novae: Tomaney, A.B. & Shafter, A.W. 1992, ApJS, 81, 683
3. General reference for extragalactic novae: Artiukhina, N.M. et al. 1995, General Catalogue of Variable Stars, Vol. V.
Extragalactic Variable Stars (Kosmosinform, Moscow)
Table 17.5. Element abundances in novae (mass fraction).
Object
Year
X
Y
T Aur
RR Pic
DQ Her
DQ Her
HR Del
V1500 Cyg
V1500 Cyg
V1668 Cyg
V693 CrA
V693 CrA
V1370 Aql
GQ Mus
PW Vul
PW Vul
QU Vul
QU Vul
V842 Cen
V827 Her
QV Vul
V2214 Oph
V977 Sco
V433 Sct
LMC 1990 No. 1
V351 Pup
1891
1925
1934
1934
1967
1975
1975
1978
1981
1981
1982
1983
1984
1984
1984
1984
1986
1987
1987
1988
1989
1989
1990
1991
0.47
0.53
0.34
0.27
0.45
0.49
0.57
0.45
0.29
0.40
0.053
0.37
0.69
0.62
0.30
0.36
0.41
0.36
0.68
0.34
0.51
0.49
0.53
0.37
0.40
0.43
0.095
0.16
0.48
0.21
0.27
0.23
0.32
0.21
0.088
0.39
0.25
0.25
0.60
0.19
0.23
0.29
0.27
0.26
0.39
0.45
0.21
0.25
C
0.0039
0.045
0.058
0.070
0.058
0.047
0.046
0.0040
0.035
0.0080
0.0033
0.018
0.0013
0.12
0.087
0.014
0.0056
N
O
0.079
0.022
0.23
0.29
0.027
0.075
0.041
0.14
0.080
0.069
0.14
0.125
0.049
0.068
0.018
0.071
0.21
0.24
0.010
0.31
0.042
0.053
0.069
0.064
0.051
0.0058
0.29
0.22
0.047
0.13
0.050
0.13
0.12
0.067
0.051
0.095
0.014
0.044
0.039
0.19
0.030
0.016
0.041
0.060
0.030
0.0070
0.10
0.19
Ne
0.011
0.0030
0.023
0.0099
0.0068
0.17
0.23
0.52
0.0023
0.00066
0.00014
0.040
0.18
0.00090
0.00066
0.00099
0.017
0.026
0.00014
0.049
0.11
Z
Ref.
0.13
0.043
0.57
0.57
0.077
0.30
0.16
0.32
0.39
0.39
0.86
0.24
0.067
0.13
0.10
0.44
0.36
0.35
0.053
0.40
0.10
0.062
0.26
0.38
[1]
[2]
[3]
[4]
[5]
[6]
[7]
[8]
[9]
[10]
[11]
[12]
[13]
[14]
[15]
[16]
[17]
[17]
[17]
[17]
[17]
[17]
[18]
[19]
Sp.-V/AQuan/1999/10/28:17:09
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17.1 T YPES OF C ATACLYSMIC VARIABLES / 437
Table 17.5. (Continued.)
Object
Year
X
Y
C
N
O
V838 Her
V838 Her
V1974 Cyg
V1974 Cyg
Solar
1991
1991
1992
1992
0.80
0.60
0.30
0.19
0.705
0.093
0.31
0.52
0.32
0.275
0.018
0.010
0.015
0.019
0.012
0.023
0.085
0.001
0.0032
0.0021
0.10
0.29
0.010
0.003
Ne
0.068
0.056
0.037
0.11
0.002
Z
Ref.
0.11
0.09
0.18
0.49
0.020
[20]
[10]
[21]
[16]
[22]
References
1. Gallagher, J.S. et al. 1980, ApJ, 237, 55
2. Williams, R.E., & Gallagher, J.S. 1979, ApJ, 228, 482
3. Williams, R.E. et al. 1978, ApJ, 224, 171
4. Petitjean, P., Boisson, C., & Pequignot, D. 1990, A&A, 240, 433
5. Tylenda, R. 1978, AcA, 28, 333
6. Ferland, G.J., & Shields, G.A. 1978, ApJ, 226, 172
7. Lance, C.M., McCall, M.L., & Uomoto, A.K. 1988, ApJS, 66, 151
8. Stickland, D.J. et al. 1981, MNRAS, 197, 107
9. Williams, R.E., Ney, E.P., Sparks, W.M., Starrfield, S., Wyckoff, S., & Truran, J.W. 1985, MNRAS, 212, 753
10. Vanlandingham, K., Starrfield, S., & Shore, S.N. 1997, MNRAS, 290, 87
11. Snijders, M.A.J. et al. 1987, MNRAS, 228, 329
12. Morisset, C., & Pèquignot, D. 1996, A&A, 312, 135
13. Saizar, P., Starrfield, S., Ferland, G.J., Wagner, R.M., Truran, J.W., Kenyon, S.J., Sparks, W.M., Williams, R.E.,
& Stryker, L.L. 1991, ApJ, 367, 310
14. Schwarz, G.J., Starrfield, S., Shore, S.N., & Hauschildt, P.H. 1997, MNRAS, 290, 75
15. Saizar, P., Starrfield, S., Ferland, G.J., Wagner, R.M., Truran, J.W., Kenyon, S.J., Sparks, W.M., Williams, R.E.,
& Stryker, L.L. 1992, ApJ, 398, 651
16. Austin, S.J., Wagner, R.M., Starrfield, S., Shore, S.N., Sonneborn, G., & Bertram, R. 1996, AJ, 111, 869
17. Andreä, J., Drechsel, H., & Starrfield, S. 1994, A&A, 291, 869
18. Vanlandingham, K., Starrfield, S., Shore, S.N., & Sonneborn, G. 1999, MNRAS, 308, 577
19. Saizar, P., Pachoulakis, I., Shore, S.N., Starrfield, S., Williams, R.E., Rotschild, E., & Sonneborn, G. 1996,
MNRAS, 279, 280
20. Vanlandingham, K.M., Starrfield, S., Wagner, R.M., Shore, S.N., & Sonneborn, G., 1996, MNRAS, 282, 563
21. Hayward, T.L., Saizar, P., Gehrz, R.D., Benjamin, R.A., Mason, C.G., Houck, J.R., Miles, J.W., Gull, G.E., &
Schoenwald, J. 1996, ApJ, 469, 854
22. Anders, E., & Grevesse, N. 1989, Geochimica et Cosmochimica Acta, 53, 197
Table 17.6. Recurrent novae.a
αb
(2000)
δb
(2000)
Name
hr
min
sec
deg
min sec
LMC 1990 #2
T Pyx
T CrB
U Sco
RS Oph
V745 Sco
V394 CrA
V3890 Sgr
V1017 Sgr
05
09
15
16
17
17
18
18
18
09
04
59
22
50
55
00
30
32
58.40
41.47
30.09
30.68
13.08
22.13
25.97
43.32
04.30
−71
−32
+25
−17
−06
−33
−39
−24
−29
39
22
55
52
42
14
00
01
23
51.6
47.0
11.4
42.1
28.4
58.3
35.1
08.6
12.8
lc
(deg)
bc
(deg)
Years of
recorded outbursts
283.04
256.76
42.43
357.29
19.48
357.02
352.50
8.85
4.15
−33.49
+9.51
+48.66
+22.47
+10.96
−3.40
−7.13
−5.84
−8.50
1968, 1990
1890, 1902, 1920, 1944, 1966
1866, 1946
1863, 1906, 1936, 1979, 1987
1898, 1933, 1958, 1967, 1985
1937, 1989
1949, 1987
1962, 1990
1901, 1919, 1973
Notes
a Three possible recurrent novae have been found in M31. Two are recorded by Rosino, L. 1973, A&AS, 9, 347, and
all three (M31 V0609, M31 V0665, and M31 V0979) by Artiukhina, N.M. et al. 1995, General Catalogue of Variable
Stars, Vol. V. Extragalactic Variable Stars (Kosmosinform, Moscow).
b Adapted from Duerbeck, H.W., 1987, Sp. Sci. Rev., 45, 1, and precessed to equinox 2000.
c Galactic coordinates.
Sp.-V/AQuan/1999/10/28:17:09
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438 / 17
C ATACLYSMIC AND S YMBIOTIC VARIABLES
Table 17.7. Recurrent novae data.
t3a
Name
(days)
Vmax
Vmin
Av
(mag.)
Distance
(kpc)
LMC 1990 #2
T Pyx
T CrB
U Sco
RS Oph
V745 Sco
V394 CrA
V3890 Sgr
V1017 Sgr
<7
88
6.8
5
9.5
14.9
5.0
17
130
11.7
7.0
2.0
8.9
4.6
9.6
7.0
8.2
7.0
> 20
15.2
10.2
17.9
11.5
19.0
18.0
17.0
13.6
∼ 0.45
∼ 1.0
∼ 0.35
0.6
2.3
∼3
∼3
1.5
1.2
55
>1
1
∼ 15:
< 1.3
4.6
> 10:
∼5
2
Spectral type
secondary
Periodb
(days)
Refs.
?
?
M4.1 ± 0.1 III
G3
K5.7 ± 0.4 I–III
M4/5 III
K
M5 III
G5 III
∼ 0.1
227.5
1.23
460
?
0.7577
?
5.7
[1, 2]
[3–6]
[3, 5,7–9]
[3–5]
[3, 5,10–13]
[5, 14, 15]
[4, 5,16]
[5, 14, 17]
[3, 5,18]
Notes
a The time for the visual light curve to fall three magnitudes after maximum.
b Orbital period.
References
1. Shore, S.N. et al. 1991, ApJ, 370, 193
2. Sekiguchi, K. et al. 1990, MNRAS, 245, 28P
3. Webbink, R.F. et al. 1987, ApJ, 314, 653
4. Schaefer, B.E. 1990, ApJ, 355, L39
5. Duerbeck, H.A. 1987, A Reference Catalog and Atlas of Galactic Novae (Reidel, Dordrecht)
6. Schaefer, B.E. et al. 1992, ApJS, 81, 321
7. Kenyon, S.J., & Garcia, M. 1986, AJ, 91, 125
8. Selvelli, P.L., Cassatella, A., & Gilmozzi, R. 1992, ApJ, 393, 289
9. Shore, S.N., & Aufdenberg, J.P. 1993, ApJ, 416, 355
10. Bode, M. 1987, RS Oph (1985) and the Recurrent Nova Phenomenon (VNU Science, Utrecht)
11. Garcia, M.R. 1986, AJ, 91, 1400
12. Dobrzycka, D., & Kenyon, S.J. 1994, AJ, 108, 2259
13. Shore, S. et al. 1996, ApJ, 456, 717
14. Harrison, T.E. et al. 1993, AJ, 105, 320
15. Sekiguchi, K. et al. 1990, MNRAS, 246, 78
16. Sekiguchi, K. et al. 1989, MNRAS, 236, 611
17. Gonzalez-Riestra, R. 1992. A&A, 265, 71
18. Sekiguchi, K. 1992, Nature, 358, 563
Table 17.8. Dwarf novae.
(1)
Namea,b
(alt. name)
WW Cet
RX And
HT Cas
FO And
WX Cet
(N Cet 1963)
TY Psc
AR And
WX Hyi
UV Per
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11) (12) (13)
Coord.c
(2000.0)
DN
Porb
Vmin
Vmax
trec
Incl.
MWD
XRS
EC
QP
0.85
0.11
1.14
0.33
0.62
0.04
1.62d
1.41e
3.0d
N
N
N
Y
N
Y
Y
Y
0.7d
1.64e
N
Y
Y
Y
N
N
N
N
N
450
N
N
N
N
N
12.2 11–35
370
11.0
25
N
N
N
N
N
N
N
N
N
N
0.30d
0.82e
N
N
N
Y
N
N
N
N
N
0 11 24.77
−11 28 42.7
1 04 35.55
41 17 58.0
1 10 12.98
60 04 35.9
1 15 32.14
37 37 35.5
1 17 04.17
−17 56 23.0
1 25 39.35
32 23 09.7
1 45 03.27
37 56 33.3
2 09 50.65
−63 18 39.9
2 10 08.25
57 11 20.6
Z
0.1765
15.0
9.3
31
Z
0.209893 12.6
10.9
5–20
SU
0.073647 16.4
SU
0.071
17.5
10.8 30–35
430
13.5
0.052:
17.5
SU
0.068:
15.3
U
0.19:
16.9
9.5
SU
0.074813 14.7
12.5
SU
0.0622:
11.7
17.5
14
140
360
54
4
51
9
81
40 0.9
10 0.3
(14)
WD
SP Wind
(15)
Spect.
type
sec.
···
···
···
···
···
···
···
···
···
···
···
···
···
···
···
···
···
···
Sp.-V/AQuan/1999/10/28:17:09
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17.1 T YPES OF C ATACLYSMIC VARIABLES / 439
Table 17.8. (Continued.)
(1)
Namea,b
(alt. name)
CP Eri
GK Per
(N Per 1901)
AF Cam
VW Hyi
AH Eri
TU Men
AQ Eri
FS Aur
CN Ori
SS Aur
CW Mon
HL CMa
(1E0643-1648)
IR Gem
AW Gem
BV Pup
U Gem
Z Cha
YZ Cnc
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11) (12) (13)
Coord.c
(2000.0)
DN
Porb
Vmin
Vmax
trec
Incl.
MWD
XRS
EC
QP
U
0.01995
N
N
Y
N
N
∼ 18d
N
Y
N
N
N
N
N
N
N
N
Y
Y
N
N
Y
N
N
N
N
N
N
Y
N
N
N
N
N
3 10 32.76
−09 45 05.3
3 31 11.82
43 54 16.8
3 32 15.59
58 47 22.1
4 09 11.34
−71 17 41.1
4 22 38.10
−13 21 30.2
4 41 40.71
−76 36 46.3
5 06 13.04
−04 08 07.0
5 47 48.34
28 35 11.1
5 52 07.77
−05 25 00.7
6 13 22.44
47 44 25.7
6 36 54.53
00 02 16.3
6 45 17.21
−16 51 35.4
6 47 34.58
28 06 22.7
7 22 40.83
28 30 16.1
7 49 05.26
−23 34 00.7
7 55 05.29
22 00 05.7
8 07 28.30
−76 32 01.3
19.7
16.5
DN 1.996803 10.2
0.2
DN 0.23:
< 73 0.90
0.20
17.0
13.4
75
SU
0.074271 13.4
9.5
27
179
U
18.4
13.5
60 0.63
10 0.15
0.20d
0.71e
1.0 F f
(14)
WD
SP Wind
SU
0.1176
> 16
11.6
SU
0.06094
17.7
12.5
U
0.059:
16.2
14.4
N
N
N
N
N
< 0.32F f
N
Y
N
N
N
N
N
N
Y
122
N
Y
N
N
N
17
∼ 1.20d
1.50e
N
N
N
Y
N
N
N
N
N
N
N
N
N
N
0.55e
N
N
N
N
∼ 0.18d
0.40e
0.87 F f
1.97F e
0.08e
0.24d
0.95e
∼ 3.1d
1.13e
2.1F f
18.7e
N
Y
Y
Y
N
Y
Y
Y
N
N
Y
N
Y
N
N
N
N
N
Y
N
Y
Y
N
N
N
0.32e
Y
Y
N
N
1.01e
N
N
N
N
37
194
40:
U
0.163199 14.2
11.9
8–22
U
0.1828
14.5
10.5 40–75
U
0.1762
16.3
11.9
Z
0.2145
13.2
11.7
SU
0.0684
16.3
SU
0.0762
18.8
11.7 22–48
150
13.8
98
410
13.1
19
U
0.225:
U
0.176906 14.0
9.1
118
SU
0.074499 15.3
12.4
82
287
8 10 56.62 SU 0.0868
28 08 33.6
SU UMa
8 12 28.20 SU 0.07635
62 36 22.6
Z Cam
8 25 13.20 Z 0.289840
73 06 39.4
AT Cnc
8 28 36.92 Z 0.238691
(Ton 323)
25 20 02.6
SW UMa
8 36 42.80 SU 0.056815
53 28 38.2
EI UMa
8 38 21.98 U 0.26810
(PG0834+488)
48 38 01.7
BZ UMa
8 53 44.14 DN 0.0679
57 48 41.1
CU Vel
8 58 32.87 SU 0.0773
−41 47 50.8
SY Cnc
9 01 03.35 Z 0.380
17 53 56.1
AR Cnc
9 22 07.48 U? 0.2146
31 03 14.6
DV UMa
9 46 36.67 SU? 0.08597
(US 943)
44 46 45.1
X Leo
9 51 01.51 U 0.1644
11 52 31.1
OY Car
10 06 22.43 SU 0.063121
−70 14 04.9
CH UMa
10 07 00.57 U 0.3448:
(PG10030+678)
67 32 46.5
DO Leo
10 40 51.21
0.234515
(PG1038+155)
15 11 33.7
15.6
14.1
14.2
13.6
15.0B
16.5
11.9
6–16
134
12.2 5–33
160
10.5 19–28
12.7B
65 0.6
10
67
3
38
16
0.74
0.10
1.08
0.40
45: 1.0:
69.7
0.7
81.8
0.1
1.12
0.13
0.84
0.09
38 0.82
3 0.05
57 0.99
11 0.15
14
10.6
459
45 0.71
18 0.22
14.9B
17.8
10.5
N
N
N
N
N
15.5
10.7
N
N
N
N
N
< 0.51F f
N
Y
N
Y
13.5
113
386
11.1 22–35
18.7
15.3
N
Y
N
N
N
18.6
15.4
N
N
N
N
N
15.8
12.4
< 0.21F f
N
Y
N
N
15.3
12.4 25–50
300
10.7
204
0.11e
Y
N
Y
N
N
N
N
N
N
N
N
N
N
N
15.9
16.0B
26 0.89
6 0.28
8–38
82.6
0.1
21.0
4.0
0.90
0.04
1.95
0.30
(15)
Spect.
type
sec.
···
···
K0-4
···
···
···
···
···
···
···
···
···
···
···
···
···
M4-5
···
M1-5
···
M3-5
···
···
···
···
···
···
···
···
···
M4.5
···
M5.5
···
···
···
···
···
···
K7
···
···
···
···
···
···
···
M5.5
···
···
···
G8-9
···
M4-5
···
M4.5
···
M2
···
M6
···
···
···
···
···
Sp.-V/AQuan/1999/10/28:17:09
Page 440
440 / 17
C ATACLYSMIC AND S YMBIOTIC VARIABLES
Table 17.8. (Continued.)
(1)
Namea,b
(alt. name)
CY UMa
V436 Cen
V442 Cen
RZ Leo
T Leo
DO Dra
(PG1140+719)
TW Vir
AL Com
BV Cen
LY Hya
(1329-294)
UZ Boo
TT Boo
EK TrA
DM Dra
BR Lup
SS UMi
(PG1551+719)
AH Her
V2051 Oph
V426 Oph
UZ Ser
BD Pav
AY Lyr
EM Cyg
AB Dra
EY Cyg
UU Aql
V4140 Sgr
(NSV 12615)
RZ Sge
WZ Sge
CM Del
V503 Cyg
VW Vul
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11) (12) (13)
Coord.c
(2000.0)
DN
Porb
Vmin
Vmax
trec
Incl.
MWD
XRS
EC
QP
N
N
N
N
N
N
Y
N
N
N
N
Y
N
N
0.41e
N
N
N
N
N
N
N
N
N
N
N
Y
N
N
0.38d
N
N
N
Y
N
N
Y
N
N
3d
N
N
N
N
N
N
N
N
N
N
N
N
N
N
N
N
Y
N
N
Y
N
N
N
N
N
N
N
N
N
N
N
N
N
N
N
N
N
N
N
N
Y
N
Y
N
Y
Y
N
N
1.07e
N
N
N
N
N
N
N
N
N
N
Y
N
N
N
< 0.27F f
30.1e
4d
N
N
N
N
Y
Y
N
N
1.6d
3.62e
N
N
N
N
Y
N
N
N
N
N
N
N
N
N
N
Y
N
N
N
N
N
N
N
N
∼ 0.30d
0.21e
N
Y
Y
Y
Y
N
N
N
N
N
N
N
N
N
N
N
N
N
N
10 56 57.05 SU 0.0583
17.0
11.9
115:
49 41 18.7
297:
11 14 00.10 SU 0.062501 15.3
12.4
22
65: 0.7:
335
5 0.1
−37 40 48.6
11 24 51.92 U 0.46:
16.5
11.9 14–39
−35 54 37.7
11 37 22.30 SU? 0.0708
19.0
11.5
01 48 57.8
11 38 26.96 SU 0.058819 15.2
11.0
450
65 0.16
03 22 08.1
19 0.04
11 43 38.34
0.165
15.6B 10.6B
42 0.83
71 41 20.4
5 0.18
11 45 21.13 U 0.18267 15.8
12.1 15–44
43 0.91
−04 26 05.9
13 0.25
12 32 25.90
0.061:
20.8
12.8
225:
14 20 42.5
13 31 19.55 U 0.610116 12.6
10.5
150
62 0.83
−54 58 33.6
5 0.10
13 31 53.84
0.13695 14.4
−29 40 59.1
14 44 01.30
0.125:
19.B
11.5
360:
22 00 56.0
14 57 44.74 SU 0.077:
< 15.6
12.7
45
40 43 42.2
15 14 01.47 SU 0.0636
> 17
12.1
231
487
−65 05 31.3
15 34 12.13 U 0.087:
20.8
15.5
59 48 31.9
15 35 53.15 SU 0.0793
> 17.5
13.1
−40 34 05.5
15 51 22.24 U 0.088:
16.9
12.6 30–48
71 45 11.9
16 44 09.99 Z 0.258116 13.9
11.3 7–27
46 0.95
25 15 02.1
3 0.10
17 08 19.09 U? 0.062428 15.0
13.0
80.5 0.44
2.0 0.05
−25 48 30.8
18 07 51.71 Z 0.2853
11.5
17–55
57 0.9
05 51 48.5
11 0.15
18 11 24.90 U 0.1730
15.5
11.9 10–40
−14 55 33.9
18 43 11.90 U 0.17930 15.4
12.4
> 55
−57 30 44.2
18 44 26.73 SU 0.07340 18.4B
13.2 8–43
37 59 51.8
205
19 38 40.10 Z 0.290909 13.3
12.5 13–46
63 0.57
30 30 28.0
10 0.08
19 49 06.50 Z 0.15198 14.5
12.3 8–22
77 44 23.5
19 54 36.77 U 0.18123: 15.5
11.4
96
32 21 54.7
19 57 18.68 U 0.14049: 16.1
11.0
71
−09 19 20.8
19 58 49.71 SU? 0.061430 17.5
15.5
−38 56 12.3
20 03 18.49 SU 0.0686
16.9
12.8 62–93
17 02 52.6
266
20 07 36.40 SU 0.056688 14.9
7.0:
72 0.8:
17 42 15.4
11876
2 0.3
20 24 56.92 U 0.162
13.4
73: 0.48
17 17 54.3
15.3
47 0.15
20 27 17.44 SU 0.07599 17.4
13.4
28
43 41 23.1
20 57 45.08 U? 0.0731
13.6
14–29
44 0.24
25 30 26.0
12 0.06
8.3 F f
0.48F f
2.38e
(14)
WD
SP Wind
(15)
Spect.
type
sec.
···
···
···
···
···
···
···
···
···
···
M3-5
···
M2-4
···
···
···
G5-8
···
···
···
···
···
···
···
···
···
···
···
···
···
···
···
K2-M0
···
···
···
K2-4
···
···
···
···
···
···
···
K5
···
···
···
K0
···
···
···
···
···
···
···
···
···
···
···
···
···
···
···
Sp.-V/AQuan/1999/10/28:17:09
Page 441
17.1 T YPES OF C ATACLYSMIC VARIABLES / 441
Table 17.8. (Continued.)
(1)
Namea,b
(alt. name)
VY Aqr
SS Cyg
RU Peg
TY PsA
(PS 74)
GD 552
IP Peg
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11) (12) (13)
Coord.c
(2000.0)
DN
Porb
Vmin
Vmax
trec
Incl.
MWD
XRS
EC
QP
SU
0.06312
3.96e
N
N
N
N
U
0.275130 11.4
8.2 24–63
N
Y
Y
Y
U
0.3746
12.7
9.0 75–85
N
Y
N
Y
SU
0.08400
16.0
86 F f
1.12e
18.2d
7.90e
N
N
Y
N
N
0.07134
16.5
20: 1.4:
N
N
N
N
N
68 1.15
0.10
N
Y
N
N
N
21 12 09.20
−08 49 36.5
21 42 42.66
43 35 09.5
22 14 02.58
12 42 11.4
22 49 39.86
−27 06 54.2
22 50 39.64
63 28 39.3
23 23 08.60
18 24 59.4
U
17.1
0.158206 14.0
18.5B
8.0B
37
5
33
5
1.19
0.02
1.21
0.19
12.0
12.B
95
(14)
WD
SP Wind
(15)
Spect.
type
sec.
···
···
K5
···
K2-3
···
···
···
···
···
M4
···
Key definitions of columns
(1) System name. (2) Right ascension, declination (Equinox 2000.0). (3) Dwarf nova sub-type, U Gem, Z Cam (standstills),
SU UMa (superoutbursts), DN (undetermined subtype). (4) Orbital period in days (spectroscopic period), colon indicates
uncertain value as adapted from [1]. (5) Vmin : minimum visual brightness in quiescence, B denotes a B magnitude
measurement (adapted from [1, 2]). (6) Maximum visual brightness peak at dwarf nova outburst (adapted from [1, 2]).
(7) Recurrence time of dwarf nova outbursts in days; the second entry is the approximate recurrence time of super outbursts
in the case of SU UMa systems (adapted from [1]). (8) Orbital inclination in degrees; second entry is the ± error estimate in
degrees (adapted from [1]). (9) Mass determination for the white dwarf in solar masses; the second entry is ± error estimate
(adapted from [3] and [1]). (10) X-ray data. If the system is a detected hard-X-ray source (0.1–4 keV) with the Einstein
Observatory (HEAO-B) imaging proportional counter (IPC) [4–7] or has an upper limit detection, then an X-ray luminosity
is given in units of 1031 ergs/s when a distance estimate is available, otherwise a count rate. If the system is a detected X-ray
source with the EXOSAT (2–20 keV) medium energy (ME) experiment [8] or is an upper limit detection, then an X-ray
luminosity is given in units of 1031 ergs/s. If the system is a detected Einstein IPC source but with no distance estimate,
then a count rate is given followed by an F. If the entry is N, then the system has not been observed with either Einstein
or EXOSAT, but ROSAT data may exist. (11) Does the system undergo eclipses, yes (Y) or no (N)? (12) Does the system
exhibit quasiperiodic oscillations (QPO), yes or no? (13) Is the underlying white dwarf detected spectroscopically during
dwarf nova quiescence (i.e., dominates the light in the far UV, EUV (IUE, HST, HUT, EUVE) and/or in the optical), yes
or no [9–13] and references therein? (14) Does the system exhibit direct spectroscopic evidence of wind outflow (e.g., P
Cygni line structure/shortward-shifted absorption or broad wind emission, during dwarf nova outburst), yes or no [14] and
references therein? (15) Spectral type of the cool, normally main sequence, lower mass, secondary star, if known.
Notes
a Finding charts for dwarf nova systems are given in [2]. Other references to finding charts are in [1] and [15].
b References to the key ground-based and space-based spectroscopic studies of dwarf novae are given in [1, 2, 15, 16] and
references therein.
c Coordinates for equinox 2000.0 adapted from [1, 2]. Coordinates for 2000.0 measured off the Space Telescope Guide
Star plates are given in [2].
d Einstein IPC X-ray luminosity.
e EXOSAT ME data.
f Einstein IPC observed flux.
Informative and stimulating reviews of virtually all aspects of dwarf novae can be found in [13, 14, 17–22].
References to original spectroscopy can be found in [1, 14–18, 21].
References
1. Ritter, H. 1990, A&AS, 85, 1179
2. Downes, R.A., Webbink, R.F., & Shara, M.M. 1997, PASP, 109, 345
3. Webbink, R.E. 1990, in Accretion-Powered Compact Binaries, edited by C. Mauche (Cambridge University Press,
Cambridge), p. 177
4. Córdova, F.M., & Mason, K.O. 1984, MNRAS, 206, 879
5. Eracelous, M., Halpern, J., & Patterson, J., 1991, ApJ, 370, 330
6. Eracelous, M., Halpern, J., & Patterson, J., 1991, ApJ, 382, 290
7. Patterson, J., & Raymond, J. 1985, ApJ, 292, 535
8. Mukai, K., & Shiokawa, K. 1993, ApJ, 418, 803
9. Panek, R., & Holm, A. 1984, ApJ, 277, 700
Sp.-V/AQuan/1999/10/28:17:09
Page 442
442 / 17
C ATACLYSMIC AND S YMBIOTIC VARIABLES
10. Sion, E.M. 1987, in The 2nd Conference on Faint Blue Stars, IAU Coll. No. 95, edited by A.G.D. Philip, D. Hayes, and
J. Liebert (Davis, Schenectady), p. 413
11. Smak, J. 1992, AcA, 42, 323
12. Long, K. et al. 1993, ApJ, 405, 327
13. La Dous, C. 1991, A&AS, 252, 100
14. Patterson, J. 1984, ApJS, 54, 443
15. Williams, G. 1983, ApJS, 53, 523
16. Szkody, P. 1987, ApJS, 63, 685
17. Robinson, E.L. 1980, ARA&A, 14, 119
18. Córdova, F.M. 1995, X-Ray Binaries, edited by W.H.G. Lewin, J. van Paradijs, and E.P.J. van den Heuvel (Cambridge
University Press, Cambridge)
19. Verbunt, F. 1986, in The Physics of Accretion onto Compact Objects, edited by M.G. Watson and N.E. White (SpringerVerlag, Berlin), p. 59
20. Wade, R. 1985, Interacting Binaries, edited by P.P. Eggleton and J.E. Pringle (Reidel, Dordrecht)
21. Warner, B. 1995, Cataclysmic Variable Stars (Cambridge University Press, Cambridge)
22. Szkody, P. 1985, in Cataclysmic and Low Mass X-Ray Binaries, edited by D.Q. Lamb and J. Patterson (Reidel, Dordrecht),
p. 385
Table 17.9. Selected list of nova-likes.
Name
(alt. names)
Coord.a
(2000)
TT Ari
(BD+14◦ 341)
RW Tri
02 06 53.09
+15 17 43.0
02 25 36.14
+28 05 51.4
08 15 18.90
−49 13 18.3
10 19 56.63
−08 41 56.0
11 05 42.80
−68 37 58.0
147.69
−44.05
146.34
−30.59
264.80
−8.09
251.32
38.28
293.35
−7.79
13 36 40.97
+51 54 50.3
MV Lyr
19 07 16.30
(MacRAE+43◦ 1) +44 01 08.4
V3885 Sgr
19 47 40.54
−42 00 25.5
(CD–42◦ 14462)
V794 Aql
IX Vel
(CPD–48◦ 1577)
RW Sex
(BD–7◦ 3007)
QU Car
(HDE 310376)
(CD–67◦ 1010)
UX UMa
VY Scl
(PS 141)
(SPC Var4)
20 17 33.97
−03 39 51.0
23 29 00.45
−29 46 46.0
Galactic Vmax b
coord.
Vmin
B−V
E(B − V )c
9.5
16.3
12.6
15.6
9.1
10.0
10.4
10.8
11.1
11.5
−0.04 [1]
0.0 [2]
0.02 [1]
0.10 [2]
107.67
63.91
74.61
16.08
357.32
−27.14
12.7
14.1
12.1
18.0
9.6
10.3
0.07 [1]
0.0 [2]
−0.13 [1]
−0.35 [1]
0.0 [1]
0.0 [2]
39.38
−20.22
19.84
−71.14
13.7
20.2
12.9
18.5
0.15 [1]
0.25 [9]
0.1 [2]
−0.03 [13] 0.03 [13]
Second.
spectral
classd
K5V
[10]
−0.04 [24] 0.0 [2]
Periode
(d)
0.137 551 [3, 4]
0.1329 [5, 6]
0.231 883 297
[11, 12]
0.193 929
[14, 15]
0.245 07 [25]
Rapid
oscillation
period (s)
1000–1600 [3, 8]
QPO [7]
[11]
VY
UX
[14, 23] UX
620, 1280
QPO [26]
[24, 25] UX
[27]
28-30
QPO [32]
2800
QPO [36]
29–30
[38, 41]
0.32 [19] 0.0 [2]
0.196 671 26
[30, 31]
0.1336 [35]
0.1379 [36]
0.206–0.259
[38, 39]
0.2163 [40]
0.23? [20]
−0.10 [16] 0.06 [16]
0.1662 [17]
∼ 500
QPO [18]
0.0 [2]
Type
[16–22]
0.454 [27]
0.113 47? [28]
K8VM6V [29]
M5V
[35]
Spec. f
Refs.
[33, 34] UX
[35, 37] VY
[39]
UX
[21, 42] VY
[17, 19] VY
Notes
a Adapted from [43].
b The range in magnitudes is taken from [44].
c The color excess, E(B − V ), is assumed to be related to the visual interstellar extinction, A , by A = 3.2 E(B − V ).
v
v
d The secondary spectral types are from spectroscopic or photometric observations and do not include estimates from mass
determinations.
e The spectroscopic period is the first entry while the photometric period is the second if it is different. Orbital parameters
can usually be found in the reference for the spectroscopic period.
f Only optical references are given. Surveys or catalogues of nova-likes exist in the infrared [45], visual [1, 46, 47],
ultraviolet [2, 48, 49], far ultraviolet [50], and X-ray [51, 52] spectral regions. References of observations for individual
nova-likes can be found in [43, 53, 54] and finding charts in [43, 46].
Sp.-V/AQuan/1999/10/28:17:09
Page 443
17.1 T YPES OF C ATACLYSMIC VARIABLES / 443
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17. Hutchings, J.B., & Cowley, A.P. 1984, PASP, 96, 559
18. Burrell, J.F., & Mould, J.R. 1973, PASP, 85, 627
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36. Borisov, G.V. 1992, A&A, 261, 154
37. Voikhanskaya, N.F. 1988, A&A, 192, 128
38. Cowley, A.P., Crampton, D., & Hesser, J.E. 1977, ApJ, 214, 471
39. Haug, K., & Drechsel, H. 1985, A&A, 151, 157
40. Metz, K. 1989, Inf. Bull. Var. Stars, 3385
41. Hesser, J.E., Lasker, B.M., & Osmer, P.S. 1974, ApJ, 189, 315
42. Honeycutt R.K., & Schlegel, E.M. 1985, PASP, 97, 1189
43. Downes, R.A., Webbink, R.F., & Shara, M.M. 1997, PASP, 109, 345
44. Ritter, H. 1990, A&AS, 85, 1179
45. Szkody, P. 1977, ApJ, 217,140
46. Williams, G. 1983, ApJS, 53, 523
47. Honeycutt, R.K., Kaitchuck, R.H., & Schlegel, E.M. 1987, ApJS, 65, 451
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49. la Dous, C. 1991, A&A, 252, 100
50. Polidan, R.S., Mauche, C.W., & Wade, R.A. 1990, in Accretion-Powered Compact Binaries, edited by C.W. Mauche
(Cambridge University Press, Cambridge), p. 77
51. Patterson, J., & Raymond, J.C. 1985, ApJ, 292, 535
52. Eracleous, M., Halpern, J., & Patterson, J. 1991, ApJ, 382, 290
53. Ritter, H. 1984, A&AS, 57, 385
54. Ritter, H. 1987, A&AS, 70, 335
Sp.-V/AQuan/1999/10/28:17:09
Page 444
444 / 17
C ATACLYSMIC AND S YMBIOTIC VARIABLES
Table 17.10. Synchronously rotating magnetic CVs (AM Her binaries).a
Mag. fieldc,e
Name
Coord.b
Dist.c
d
Porb
(alt. name)
(2000)
(pc)
(min)
BL Hyi
(H0139-68)
WW Hor
(EXO0234.5-5232)
EF Eri
(2A0311-227)
VY For
(EXO032957-2606.9)
UZ For
(EXO033319-2554.2)
BY Cam
(H0538+608)
VV Pup
EK UMa
(1E1048+5241)
AN UMa
ST LMi
(CW1103+254)
DP Leo
(1E1114+182)
EU UMa f
(RE1149+28)
V834 Cen
(1E1405-451)
MR Ser
(PG1550+191)
AM Herg
(3U1809+50)
EP Dra
(H1907+690)
QS Tel
(RE 1938-461)
QQ Vul
(1E2003+225)
V1500 Cyg
(Nova Cyg 1975)
CE Gru
(Grus V1)
1 41 00.25
−67 53 27.7
2 36 11.45
−52 19 13.5
3 14 13.03
−22 35 41.4
3 31 04.58
−25 56 55.5
3 35 28.61
−25 44 22.6
5 42 48.90
60 51 31.8
8 15 06.73
−19 03 16.8
10 51 35.23
54 04 36.0
11 04 25.71
45 03 15.0
11 05 39.75
25 06 28.9
11 17 16.00
17 57 41.1
11 49 55.70
28 45 07.5
14 09 07.46
−45 17 17.1
15 52 47.23
18 56 27.6
18 16 13.33
49 52 04.2
19 07 06.13
69 08 42.4
19 38 35.73
−46 12 56.5
20 05 41.93
22 39 59.1
21 11 36.61
48 09 01.9
21 37 56.38
−43 42 13.1
m v c,d
128
113.6
14–18.5
500
114.6
19–21
> 89
81.0
13.5–17.5B
228
17.5
250
126.5
18–20.5
200
201.9
199.3h
100.4
14.5–>17B
114.5
18–20
> 270
114.8
14.5–19B
128
113.9
15.0–17
145
14.5–18
> 380
89.8
17.5–19.5B
16.5B
86
90:
103:
101.5
112
113.6
15–17
14.0–17
75
185.6
12–15.5
600:
104.6
18
140.0
15.5
> 400
222.5
14.5–15.5
1000–
1400
201.0
197.5i
108.6
17–18
18–21B
B1 , B2
Bd
(MG)
(MG)
33
P
25:
P
30
Z
15
Z
10–50:
P
53, 75:
C
41:
C
31.5, 56
C
47:
C
36
C
Polarization
L sx
Circ.
Lin.
(ergs s−1 )
(%)
(%)
Refs.
1 × 1031
17
12
[1, 2]
4 × 1033
30
···
[3]
> 1 × 1032
20
9
[4, 5]
[6]
7 × 1033
6
3
[7, 8]
10
1
[9–12]
15
15
[13–15]
20
···
[16, 17]
> 3 × 1032
35
···
[18–20]
2 × 1032
20
12
[21–24]
> 1 × 1033
35
9
[25, 26]
5 × 1032
18
Z
30.5, 59
C,Z
[27]
23
Z,C
24
C
14, 28
C
10–50:
P
25–50:
P
20:, 20:
P
10
Z
22
Z
1 × 1032
30
10
[28–31]
5 × 1030
12
5
[32, 33]
9 × 1032
10
8
[34–37]
10
···
[38]
6
10
[39]
8
2
[40]
10
···
[41]
15
···
[42, 43]
> 4 × 1034
Notes
a These binaries contain accreting white dwarfs that are strongly magnetized and rotate essentially synchronously, i.e.,
rotation period within 2% of the orbital period Porb [44, 45]. They are more commonly known as AM Herculis binaries, or
polars, and are characterized by the strong optically polarized radiation they emit.
m v : Visual magnitude. B indicates blue magnitude. Nova outburst magnitude not given.
B1 , B2 are the dominant and less dominant accretion poles, respectively.
Bd is the polar field if a dipole structure is assumed to model the Zeeman features.
Z : Zeeman features.
C: Cyclotron features.
P: Magnetic field estimated from polarization.
L sx : Soft X-ray luminosity (see [46, 47] for uncertainties in the estimates).
b Adapted from [44].
c Adapted from [45].
d Adapted from [48].
e Adapted from [49].
f Shows strong He II λ4686 line and strong EUV emission, characteristics of AM Her binaries.
g Radio source.
h Rotation period.
i White dwarf presumed to have become asynchronous following nova outburst and is now synchronizing.
Sp.-V/AQuan/1999/10/28:17:09
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17.1 T YPES OF C ATACLYSMIC VARIABLES / 445
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2. Piirola, V.V., Reiz, A., & Coyne, G.V. 1987, A&A, 185, 189
3. Bailey, J., Wickramasinghe, D.T., Hough, J.H., & Cropper, M. 1988, MNRAS, 234, 19P
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5. Tapia, S. 1979, IAU Circ. 3327
6. Berriman, G., & Smith, P.S. 1988, ApJ, 329, L97
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8. Schwope, A.D., Beuermann, K., & Thomas, H.-C. 1990, A&A, 230, 120
9. Cropper, M. et al. 1989, MNRAS, 236, 29P
10. Mason, P.A., Liebert, J., & Schmidt, G.D. 1989, ApJ, 346, 941
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14. Wickramasinghe, D.T., Ferrario, L., & Bailey, J. 1989, ApJ, 342, L35
15. Piirola, V., Reiz, A., & Coyne, G.V. 1990, A&A, 235, 245
16. Cropper M., Mason, K.O., & Mukai, K. 1990, MNRAS, 243, 565
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19. Schmidt, G.D., Stockman, H.S., & Grandi, S.A. 1986, ApJ, 300, 804
20. Schwope, A.D., & Beuermann, K. 1990, A&A, 238, 173
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22. Bailey, J. et al. 1985, MNRAS, 215, 179
23. Cropper, M. 1987, Ap&SS, 131, 651
24. Shore, S.N. et al. 1982, PASP, 94, 682
25. Cropper, M., & Wickramasinghe, D.T. 1993, MNRAS, 260, 696
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Table 17.11. Asynchronously rotating magnetic CVs (DQ Her binaries).a
Name
(alt. name)
XY Ari f
(1H0253+193)
Coord.b
(2000)
2 56 08.1
19 26 34.
Dist.c
(pc)
Prot
(min)
Porb
(h)
mv d
200
3.42
6.06
12–13.5K
L hx c,e
(erg s−1 )
2 × 1032
Refs.
[1, 2]
Sp.-V/AQuan/1999/10/28:17:09
Page 446
446 / 17
C ATACLYSMIC AND S YMBIOTIC VARIABLES
Table 17.11. (Continued.)
Name
(alt. name)
Coord.b
Dist.c
(2000)
(pc)
Prot
(min)
Porb
(h)
mv d
L hx c,e
(erg s−1 )
Refs.
GK Perg
(Nova Per 1901)
V471 Tau
3 31 11.82
43 54 16.8
3 50 24.79
17 14 47.8
5 29 25.44
−32 49 04.5
5 34 50.67
−58 01 40.9
5 43 20.22
−41 01 55.2
7 31 28.98
9 56 22.6
525
5.86
47.9
10–14.0
7.4 × 1032
[3–5]
49
9.24
12.51
9–10
> 500
31.9
5.49
13.5–14
650:
126:
6.5:
14–16
> 500
31.9:
5.72
15.5
700–1000
14.1:
15.2:
28.2:
13.9:
3.24
14–14.5
∼ 6:
14.5
76–90
67.0
1.64
10–14
2.60
12.5–13B
300–500
93.8:
106.4:
1.18
4.65
14–17.5
< (1.1–3.0) × 1030
1000:
1.06
5.04
14.5–16
< 2 × 1031
540–660
12.4
3.37
12–> 17
28–78
0.55:
9.88
10–11.5
200–640
20.9
4.85
13–14
100–750
13.4
3.59
13.5–15
TV Col
(2A0526-328)
TW Pic
(H0534-581)
TX Col
(1H0542-407)
BG CMih
(3A0729+103)
PQ Gemi
(RE0751+14)
EX Hya
V795 Her f
(PG 1711+336)
DQ Her
(Nova Her 1934)
V533 Her f
(Nova Her 1963)
V1223 Sgr
AE Aqrg
FO Aqr
(H2215-086)
AO Psc
(H2252-035)
7 51 17.39
14 44 24.6
12 52 24.40
−29 14 56.7
17 12 56.09
33 31 21.4
18 07 30.17
45 51 31.9
18 14 20.34
41 51 21.3
18 55 02.24
−31 09 48.5
20 40 09.02
−0 52 15.5
22 17 55.43
−8 21 04.6
22 55 17.97
−3 10 40.4
[6–8]
> 6.1 × 1032
[9, 10]
[11]
> 2.8 × 1032
[12, 13]
(0.7–1.4) × 1033
[14–19]
[20, 21]
(0.3–1.8) × 1032
[22, 23]
[24, 25]
[26–28]
[26, 27, 29]
(0.9–1.3) × 1033
[30–33]
< (0.5–3.6) × 1030
[34–37]
(0.8–8.3) × 1032
[38–41]
(0.02–1.3) × 1033
[33, 42–44]
Notes
a These binaries are believed to contain accreting magnetized white dwarfs that rotate asynchronously with the rotation
period Prot differing by more than 2% from the orbital period Porb . They do not in general emit optically polarized radiation
and probably have magnetic fields strengths that are weaker than those found in the synchronously rotating magnetic CVs.
They are more commonly, but inconsistently, referred to as DQ Herculis binaries and/or intermediate polars. For example,
some authors refer to only those binaries with Prot 0.1Porb as DQ Hers and the others as intermediate polars. Prot is
often difficult to identify so that some of the binaries in the table should not actually belong to it. m v : Visual magnitude.
B, K indicate blue, K band magnitudes. Nova outburst magnitude not given. L hx : Hard-X-ray luminosity. The main
uncertainty is due to that in the distance.
b Adapted from [45].
c Adapted from [46, 47].
d Adapted from [48].
e Adapted from [47, 49].
f Identification as a magnetic CV uncertain. XY Ari lies behind Lynds dark cloud L 1457 and is not visible optically.
g Radio source.
h Shows weak but significant optical/IR circular polarization implying a magnetic field of roughly 4 MG.
i Shows significant optical/IR linear and circular polarization implying a magnetic field of 8–18 MG.
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5. Patterson, J. 1991, PASP, 103, 1149
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10.
11.
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22.
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25.
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Young, A., & Nelson, B. 1972, ApJ, 173, 653
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17.2
TYPES OF SYMBIOTIC VARIABLES
A symbiotic variable [2, 20–22] is a long-period (> 100 days) binary system with a detached or
semidetached cool, red giant or Mira star losing mass via a wind to a hot, luminous white dwarf
or main-sequence companion. Table 17.12 lists the positions of the best-known symbiotic stars,
Table 17.13 gives their variability, and Table 17.14 supplies their orbital parameters. The symbiotic
variables are subdivided into D(ust) types which tend to be associated with Miras and S(tar) types
which tend to be associated with red giants. Some symbiotic variables undergo a large outburst which
may be due to an accretion event or a shell flash on the hot component. These symbiotic variables are
observationally similar to the very slow novae and are called symbiotic novae [23]. Recurrent novae
which have a red giant companion may be related to the symbiotic novae [2].
Sp.-V/AQuan/1999/10/28:17:09
Page 448
448 / 17
C ATACLYSMIC AND S YMBIOTIC VARIABLES
Table 17.12. Representative symbiotic stars.a
Name
Other name
α
hr min sec
δ
deg min sec
lII
bII
EG And
AX Per
BX Mon
RX Pup
SY Mus
AG Dra
RT Ser
AR Pav
BF Cyg
CH Cyg
HM Sge
CI Cyg
V1016 Cyg
RR Tel
V1329 Cyg
AG Peg
Z And
R Aqr
HD 4174
MWC 411
AS 150
HD 69190
HD 100336
···
MWC 265
MWC 600
MWC 315
HD 182917
···
MWC 415
AS 373
Hen 1811
HBV 475
HD 207757
HD 221650
HD 222800
00 44 37.18
01 36 22.73
07 25 22.72
08 14 12.24
11 32 10.16
16 01 40.98
17 39 51.94
18 20 27.92
19 23 53.55
19 24 33.08
19 41 57.07
19 50 11.86
19 57 04.99
20 04 18.54
20 51 01.27
21 51 01.99
23 33 40.02
23 43 49.45
40 40 45.6
54 15 02.7
−03 35 50.8
−41 42 29.8
−65 25 11.2
66 48 10.3
−11 56 38.8
−66 04 41.8
29 40 29.3
50 14 29.5
16 44 39.6
35 41 03.2
39 49 36.5
−55 43 32.9
35 34 53.3
12 37 31.9
48 49 06.1
−15 17 04.4
121.5
129.5
220.0
258.5
294.8
100.3
13.9
328.5
62.9
81.8
53.6
70.9
75.2
342.2
77.8
69.3
110.0
66.5
−22.2
−8.0
5.9
−3.9
−3.8
41.0
10.0
−21.6
6.7
15.6
−3.2
4.7
5.7
−32.2
−5.5
−30.9
−12.1
−70.3
Note
a For general systems, see [1–7]. For Miras, see [8] and [9]. For multiwavelength
properties, see [10–12]. For outbursts, see [13]. For interpretation of UV spectra, see [14]
and [15].
References
1. Payne-Gaposchkin, C. 1957, The Galactic Novae (North-Holland, Amsterdam)
2. Allen, D.A. 1984, Proc. ASA, 5, 369
3. Kenyon, S.J. 1986, The Symbiotic Stars (Cambridge University Press, Cambridge)
4. Kenyon, S.J. 1992, in Evolutionary Processes in Interacting Binary Stars, IAU
Symposium No. 151, edited by Y. Kondo et al. (Kluwer Academic, Dordrecht), p. 137
5. Mikolajewska, J. et al. 1988, The Symbiotic Phenomenon, IAU Coll. 103 (Kluwer
Academic, Dordrecht) (referred to as IAU Coll. 103)
6. Garcia, M.R., & Kenyon, S.J. 1988, in The Symbiotic Phenomenon, IAU Coll. 103
(Kluwer Academic, Dordrecht), p. 27
7. Vogel, M. 1990, thesis, ETH, Zürich
8. Whitelock, P. 1987, PASP, 99, 573
9. Whitelock, P. 1988, IAU Coll. 103, p. 47
10. Ivison, R.J., et al. 1991, MNRAS, 249, 374
11. Seaquist, E.R., & Taylor, A.R. 1990, ApJ, 349, 313
12. Van Winckel, H., et al. 1993, A&AS, 102, 401
13. Mürset, U. & Nussbaumer, H. 1994, A&A, 282,586
14. Shore, S.N., & Aufdenberg, J.P. 1993, ApJ, 416, 355
15. Boyarchuk, A.A. 1993, in The Realm of Interacting Binary Stars, edited by J. Sahade,
G.E. McCulsky, and Y. Kondo (Kluwer Academic, Dordrecht), p. 189
Table 17.13. Symbiotic stars: Variability.
Name
Max
Min
Orbit
epocha
Orbit
period
Type
EG And
AX Per
BX Mon
RX Pupb
SY Mus
AG Dra
RT Ser
7.1
9.4
9.5
9.0
10.2
8.9
10.6
7.8
13.6
13.4
14.1
12.7
11.8
17.0
45 380.0
36 667.0
49 530.0
···
36 460.0
38 900.0
···
482
680.8
1401
···
621.8
554.0
···
S
S
S
D
S
S
S
Spectrum
Ecl.
Outburst
M2.4 III
M5 IIIep
M4.6ep
M5-6 IIIpe:
M2 III
K1 IIpev
M5.5 III
E
E
E?
···
E
···
···
···
1980
···
···
···
1980
1909
Refs.
[1–3]
[4]
Sp.-V/AQuan/1999/10/28:17:09
Page 449
17.2 T YPES OF S YMBIOTIC VARIABLES / 449
Table 17.13. (Continued.)
Name
Max
Min
Orbit
epocha
Orbit
period
Type
AR Pav
BF Cyg
CH Cygc
CH Cygc
HM Sgeb
CI Cyg
V1016 Cygb
RR Telb
V1329Cyg
AG Peg
Z And
R Aqrb
7.4
9.3
5.6
5.6
11.1
9.9
10.1
6.5
12.1
6.0
8.0
5.8
13.6
13.4
8.5
8.5
18.0
13.1
17.5
16.5
18.0
9.4
12.4
12.4
···
15 058.0
47 302.0
45 517.0
···
45 323.8
···
···
24 869.9
42 710.1
···
···
605
756.8
756
5294
···
855.3
···
···
964
816.5
756.9
···
S
S
S
S
D
S
D
D
S
S
S
S
Spectrum
Ecl.
Outburst
Refs.
≥ M4 III
M5 III
M6 III + WD
+?
> M4
M5 II
> M4 III
Pec
> M4 IIIp
M3 III
M3.5 III
M7 IIIpev
E
···
···
E?
···
···
···
···
E
···
E?
E?
1964
···
1964
1964
1975
1975
1963
1944
1964
1850
1985?
···
[5–7]
[8]
[8]
[9]
[10]
[11]
[12, 13]
[14]
[15]
[16]
[17]
Notes
a Date given as JD2400000+.
b Mira periods: HM Sge: 540 days; R Aqr: 387 days; RX Pup: 580 days; V1016 Cyg: 450 days; RR Tel: 387 days.
c CH Cyg is a possible triple system.
References
1. Skopal, A. et al. 1988, IAU Coll. No. 103, p. 289
2. Vogel, M. 1991, A&A, 249, 173
3. Oliversen, N. et al. 1985, ApJ, 295, 620
4. Payne-Gaposchkin, C. 1957, The Galactic Novae (North-Holland, Amsterdam)
5. Mikolajewska, J. et al. 1989, AJ, 98, 1427
6. Mikolajewska, J., & Mikolajewski, M. 1988, IAU Coll. No. 103, p. 299
7. Slovak, M. et al. 1988, IAU Coll. No. 103, p. 265
8. Hinkle, K.H. et al. 1993, AJ, 105, 1074
9. Nussbaumer, H., & Vogel, M. 1990, A&A, 101, 118
10. Kenyon, S.J. et al. 1991, AJ, 101, 637
11. Nussbaumer, H., & Schild, H. 1981, A&A, 101, 118
12. Thackeray, A.D. 1977, MNRAS, 83, 1
13. Pentson, M.V. et al. 1983, MNRAS, 202, 833
14. Nussbaumer, H., & Vogel, M. 1991, A&A, 248, 81
15. Kenyon, S. et al. 1993, AJ, 106, 1573
16. Mattei, J.A. 1978, JRASC, 72, 61
17. Kafatos, M. et al. 1986, ApJS, 62, 853
Table 17.14. Symbiotic stars: Orbital parameters.
Name
Period (days)
EG And
AX Per
BX Mona
AG Dra
AR Pav
BF Cygb
CH Cyg
CH Cyg
CI Cyg
V1329 Cyg
AG Peg
Z And
482
680.8
1401 ± 8
554.0
605
756.8
756
5294
855.3
964
816.5
756.9
e
0.043 ± 0.021
0.0:
0.49 ± 0.1
0.0:
0.11
0.3
0.0:
0.058 ± 0.035
0.0:
0.3:
0.0:
0.20 ± 0.11
f (M) (M )
0.021
0.032
0.0075
0.008
0.14
0.0014
0.057
0.027
21:
0.012
0.024
Notes
a BX Mon: mass ratio q = 6.7 ± 1.3, epoch is for cool star in front.
b BF Cyg: Mass ratio q = 1.7 ± 0.6.
Refs.
[1–5]
[6]
[7]
[8]
[9]
[10–13]
[14]
[15]
[16, 17]
[18, 19]
[1, 13, 20]
[1]
Sp.-V/AQuan/1999/10/28:17:09
Page 450
450 / 17
C ATACLYSMIC AND S YMBIOTIC VARIABLES
References
1. Kenyon, S.J. 1992, in Evolutionary Processes in Interacting Binary Stars, IAU
Symposium No. 151, edited by Y. Kondo et al. (Kluwer Academic, Dordrecht), p. 137
2. Skopal, A. et al. 1988, IAU Coll. No. 103, p. 289
3. Munari, U. et al. 1988, A&A, 198, 173
4. Vogel, M. 1991, A&A, 249, 173
5. Oliversen, N. et al. 1985, ApJ, 295, 620
6. Garcia, M.R., & Kenyon, S.J. 1988, in The Symbiotic Phenomenon, IAU Coll.
No. 103 (Kluwer Academic, Dordrecht), p. 27
7. Dumm, T., Muerset, U., Nussbaumer, H., Schild, H., Schmid, H.M., Schmutz, W.,
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8. Mikolajewska, J. et al. 1995, AJ, 109, 1289
9. Kenyon, S.J. 1986, The Symbiotic Stars (Cambridge University Press, Cambridge)
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G.E. McCulsky, and Y. Kondo (Kluwer Academic, Dordrecht), p. 189
11. Mikolajewska, J. et al. 1989, AJ, 98, 1427
12. Mikolajewska, J., & Mikolajewski, M. 1988, IAU Coll. No. 103, p. 299
13. Slovak, M. et al. 1988, IAU Coll. No. 103, p. 265
14. Hinkle, K.H. et al. 1993, AJ, 105, 1074
15. Mikolajewski, M. 1988, IAU Coll. No. 103 (Kluwer Academic, Dordrecht), p. 221
16. Kenyon, S.J. et al. 1991, AJ, 101, 637
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Systems (Copernicus Foundation for Polish Astronomy, Warsaw), p. 3
18. Vogel, M. 1990, thesis, ETH, Zürich
19. Nussbaumer, H., & Vogel, M. 1991, A&A, 248, 81
20. Kenyon, S. et al. 1993, AJ, 106, 1573
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