J/ApJ/914/5 Abundance anomalies in cataclysmic variables (Sparks+, 2021)
Nova-produced common envelope: source of the nonsolar abundances and an
additional frictional angular momentum loss in cataclysmic variables.
Sparks W.M., Sion E.M.
<Astrophys. J., 914, 5 (2021)>
=2021ApJ...914....5S 2021ApJ...914....5S
ADC_Keywords: Binaries, cataclysmic; Stars, variable; Stars, masses
Keywords: Binary stars ; Cataclysmic variable stars ; Classical novae
Abstract:
A substantial fraction of cataclysmic variables (CVs) reveal nonsolar
abundances. A comprehensive list of CVs that includes those that have
been examined for these abundances is given. Three possible sources of
these nonsolar abundances on the secondary are accretion during the
red giant common envelope phase, an evolved main-sequence secondary,
and nova-processed material. Use of the secondary's cross section just
on the escaping nova material to change the abundances of its
convective region has been the killing objection for considering
nova-processed material. The key element, ignored in other studies, is
that a thermonuclear runaway on a white dwarf causes a strong
propagating shock wave that not only ejects material but also produces
a large amount of nonejected material that forms a common envelope.
This nova-produced common envelope contains a large amount of nonsolar
material. We demonstrate that the secondary has the capacity and time
to reaccrete enough of this material to acquire a significant nonsolar
convective region. This same envelope interacting with the binary will
produce a frictional angular momentum loss, which can be the
consequential angular momentum loss needed for the average CV white
dwarf mass, the white dwarf mass accretion rates, the period minimum,
the orbital period distribution, and the space density of CV problems.
This interaction will decrease the orbital period, which can cause the
recently observed sudden period decreases across nova eruptions. A
simple, rapid evolutionary model of the secondary that includes the
swept-up nova-produced material and the increasing convective region
is developed and applied to individual CVs.
Description:
Table 1 contains all of the cataclysmic variables (CVs) whose period
and mass ratio (q) are known from the Ritter & Kolb (2003A&A...404..301R 2003A&A...404..301R ;
See B/cb) catalog (version 7.24, updated to 2015 December 31 and
additions listed in its footnote) and all of the CVs examined for
abundance anomalies. We did not include CVs whose q value is estimated
or an upper or lower limit. See Section 2 for further details.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 64 200 CVs with known periods and mass ratios or
nonsolar abundance indicators
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See also:
B/cb : Cataclysmic Binaries, LMXBs, and related objects (Ritter+, 2004)
V/113 : Cataclysmic Binaries, LMXBs, and related objects (Ritter+, 2003)
V/123 : Catalog of Cataclysmic Variables (Downes+ 2001-2006)
J/A+A/312/93 : Cataclysmic var. systemic-velocity (van Paradijs+, 1996)
J/PASP/109/441 : Northern Cataclysmic Variables (Henden+ 1997)
J/A+A/332/586 : Cataclysmic variables light curves (Bruch 1998)
J/ApJ/565/511 : Cataclysmic variables in the 2MASS 2IDR (Hoard+, 2002)
J/AJ/134/185 : Cataclysmic variables from SDSS-DR5 (Szkody+, 2007)
J/other/NewA/12.446 : Absolute magnitudes of cataclysmic variables (Ak+, 2007)
J/other/NewA/13.133 : 2MASS photometry of cataclysmic variables (Ak+, 2008)
J/PASP/122/1285 : RVels of 20 cataclysmic var. (Thorstensen+, 2010)
J/ApJS/194/28 : The evolution of cataclysmic variables (Knigge+, 2011)
J/AJ/142/181 : CVs from SDSS. VIII. The final year (Szkody+, 2011)
J/AJ/144/81 : Sp. and photometry of CV candidates (Thorstensen+, 2012)
J/MNRAS/443/3174 : 72 faint CV candidates in CRTS (Breedt+, 2014)
J/A+A/573/A61 : Photometry of new eclipsing CVs (Southworth+, 2015)
J/other/NewA/34.234 : Gal. cataclysmic variables distances (Ozdonmez+, 2015)
J/MNRAS/461/1576 : EX Hya mid-eclipse timings (Echevarria+, 2016)
J/AJ/152/226 : RVels of 35 cataclysmic variables (Thorstensen+, 2016)
J/AJ/154/252 : A VLA survey of magnetic CVs. I. The data (Barrett+, 2017)
J/MNRAS/465/4968 : Cataclysmic variables observations (Hardy+, 2017)
J/other/RAA/18.68 : Cataclysmic variables from LAMOST DR3 (Han+, 2018)
J/AJ/155/247 : RVels of 6 X-ray cataclysmic binaries (Halpern+, 2018)
J/AJ/159/43 : Sp. identified CVs from LAMOST survey. I. (Hou+, 2020)
J/AJ/159/114 : Magnetic CVs sp. & other var. objects II. (Oliveira+, 2020)
J/AJ/159/198 : CVs in the ZTF 1st-yr (2018-2019) (Szkody+, 2020)
J/AJ/160/6 : OSMOS & modspec RVs of 30 CVs (Thorstensen, 2020)
J/MNRAS/492/L40 : Disentangling CVs in Gaia DR2 (Abril+, 2020)
J/AJ/162/94 : Cataclysmic variables in ZTF 2nd year (Szkody+, 2021)
J/ApJS/257/65 : Cataclysmic variables from LAMOST DR6 (Sun+, 2021)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name System name
13 A1 --- f_Name Flag on Name (1)
15- 20 A6 --- Type CV type (2)
22- 34 F13.11 d Porb [0.0037/5.8] Orbital period (2)
36 A1 --- r_Porb Reference for Porb (3)
38- 43 F6.4 --- M2/M1 [0.02/3.8]? Mass ratio (2)
45- 50 F6.4 Msun M2 [0.01/3.4]? Secondary mass (2)
52 A1 --- N/C NV1240/CIV1541 abundance anomaly (4)
54 A1 --- 13C/12C 13C/12C abundance anomaly (4)
56- 57 A2 --- NIR NIR lines abundance anomaly (4)
59 A1 --- IRc IR continuum abundance anomaly (4)
61 A1 --- CO CO abundance anomaly (4)
63- 64 A2 --- UV UV abundance anomaly (4)
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Note (1): Orbital periods and other parameters are updated from the
references as follows:
h = Rodriquez-Gil et al. (2020MNRAS.494..425R 2020MNRAS.494..425R)
i = Echevarria et al. (2019RMxAA..55...21E 2019RMxAA..55...21E)
j = Hernandez et al. (2017MNRAS.470.1960H 2017MNRAS.470.1960H)
k = McAllister et al. (2017MNRAS.464.1353M 2017MNRAS.464.1353M)
l = McAllister et al. (2017MNRAS.467.1024M 2017MNRAS.467.1024M)
m = Miszalski et al. (2016MNRAS.456..633M 2016MNRAS.456..633M)
n = Mason et al. (2019MNRAS.488.2881M 2019MNRAS.488.2881M)
o = Pala et al. (2018MNRAS.481.2523P 2018MNRAS.481.2523P)
p = The q value and secondary mass for V396 Hya (CE315) are from
Ruiz et al. (2001ApJ...552..679R 2001ApJ...552..679R)
q = Harrison's (2018ApJ...861..102H 2018ApJ...861..102H) observations support a q=0.96 for DX And,
which we used instead of the listed 0.66.
r = The orbital parameters for EX Hya are recalculated from new observations
of K1 (Echevarria et al. 2016, J/MNRAS/461/1576).
s = The q=0.10 for MR Ser from Shahbaz & Wood (1996MNRAS.282..362S 1996MNRAS.282..362S) is
included
t = The q=0.017 for J1122-1110 from Breedt et al. (2012MNRAS.425.2548B 2012MNRAS.425.2548B) is
included
u = Although VZ Scl has a Ritter-Kolb Catalogue (B/cb) listed m2 of
1.4M☉ from Warner & Thackeray (1975MNRAS.172..433W 1975MNRAS.172..433W), a later paper
(O'Donoghue et al. 1987MNRAS.225...43O 1987MNRAS.225...43O) found m2=0.32M☉, which we
used.
v = For V1223 Sgr, Penning (1985ApJ...289..300P 1985ApJ...289..300P) and
Watts+ (1985MNRAS.215...83W 1985MNRAS.215...83W) both used a main-sequence mass-radius
relationship and found m2=0.40M☉.
Beuermann et al. (2004A&A...419..291B 2004A&A...419..291B), noting that the secondary was
bloated, commented on the effects of using an m2 of 0.25M☉.
Ritter & Kolb (2003, B/cb) adopted an m2 of 0.33±0.08M☉
to cover this mass range. For our analysis, we adopted an m2
of 0.40M☉.
w = We included QS Vir (EC 13471-1258), since it is most likely a pre-CV
just about to become a CV (O'Donaghue+ 2003MNRAS.345..506O 2003MNRAS.345..506O and
Parsons+ 2010MNRAS.407.2362P 2010MNRAS.407.2362P).
Note (2): The CV type, period, mass ratio, and secondary are from
Ritter & Kolb's (2003) catalog (see B/cb), which was last updated on
2015 December 31. This list is updated from
McAllister+ (2019MNRAS.486.5535M 2019MNRAS.486.5535M) for six new CV (CSS080623=J1404-1027,
CSS110113=J0431-0314, J0901+4809, J0945-1944, and V713 Cep, the
reanalyses of CTCV 1300 (=J1300-3052=V1258 Cen), DV UMa, GY Cnc, IY UMa,
OY Car, J1152+4049, Z Cha, J1501+5501, and J1006+2337, and a number of
improved periods. They also listed the orbital parameters of CVs from
many sources, which we included.
Note (3): If not from B/cb (see Note (2)), period reference as follows:
a = Thorstensen et al. (2017RNAAS...1...29T 2017RNAAS...1...29T)
b = Dai et al. (2017A&A...606A..45D 2017A&A...606A..45D)
c = Schwope & Thinius (2018AN....339..540S 2018AN....339..540S)
d = Schaefer (2020MNRAS.492.3343S 2020MNRAS.492.3343S)
e = Fuentes-Morales et al. (2021MNRAS.501.6083F 2021MNRAS.501.6083F)
f = Canizares et al. (2018RNAAS...2..184C 2018RNAAS...2..184C)
g = Bai et al. (2016ApJ...828...39B 2016ApJ...828...39B) - also found an AlI absorption line
doublet in the visual varied.
Note (4): Code as follows:
Y = an abundance anomaly was observed
N = an abundance anomaly was looked for but not found
V = variable feature
YH = enhanced abundances of odd-numbered nuclear species above oxygen
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 02-Dec-2022