2003PASP..115.1308P

Query : 2003PASP..115.1308P

2003PASP..115.1308P - Publ. Astron. Soc. Pac., 115, 1308-1329 (2003/November-0)

Superhumps in cataclysmic binaries. XXIV. Twenty more dwarf novae.

PATTERSON J., THORSTENSEN J.R., KEMP J., SKILLMAN D.R., VANMUNSTER T., HARVEY D.A., FRIED R.E., JENSEN L., COOK L.M., REA R., MONARD B., McCORMICK J., VELTHUIS F., WALKER S., MARTIN B., BOLT G., PAVLENKO E., O'DONOGHUE D., GUNN J., NOVAK R., MASI G., GARRADD G., BUTTERWORTH N., KRAJCI T., FOOTE J. and BESHORE E.

Abstract (from CDS):

We report precise measures of the orbital and superhump period in 20 more dwarf novae. For 10 stars, we report new and confirmed spectroscopic periods–signifying the orbital period Po–as well as the superhump period Psh. These are GX Cas, HO Del, HS Vir, BC UMa, RZ Leo, KV Dra, KS UMa, TU Crt, QW Ser, and RZ Sge. For the remaining 10, we report a medley of Po and Pshmeasurements from photometry; most are new, with some confirmations of previous values. These are KV And, LL And, WX Cet, MM Hya, AO Oct, V2051 Oph, NY Ser, KK Tel, HV Vir, and RX J1155.4-5641.

Periods, as usual, can be measured to high accuracy, and these are of special interest since they carry dynamical information about the binary. We still have not quite learned how to read the music, but a few things are clear. The fractional superhump excess {epsiv}[=(Psh-Po)/Po] varies smoothly with Po. The scatter of the points about that smooth curve is quite low, and can be used to limit the intrinsic scatter in M1, the white dwarf mass, and the mass-radius relation of the secondary. The dispersion in M1does not exceed 24%, and the secondary-star radii scatter by no more than 11% from a fixed mass-radius relation. For the well-behaved part of {epsiv}(Po) space, we estimate from superhump theory that the secondaries are 18%±6% larger than theoretical ZAMS stars. This affects some other testable predictions about the secondaries: at a fixed Po, it suggests that the secondaries are (compared with ZAMS predictions) 40%±14% less massive, 12%±4% smaller, 19%±6% cooler, and less luminous by a factor of 2.5(7). The presence of a well-defined mass-radius relation, reflected in a well-defined {epsiv}(Po) relation, strongly limits effects of nuclear evolution in the secondaries.


Abstract Copyright: ∼

Journal keyword(s): accretion, accretion disks - Stars: Binaries: Close - Stars: Novae, Cataclysmic Variables - stars: individual (AO Octantis) - Stars: Individual: Constellation Name: BC Ursae Majoris - stars: individual (GX Cassiopeiae) - stars: individual (HO Delphini) - stars: individual (HV Virginis) - stars: individual (KK Telescopii) - stars: individual (KS Ursae Majoris) - stars: individual (KV Andromedae) - stars: individual (KV Dracnonis) - stars: individual (LL Andromedae) - stars: individual (MM Hydrae) - stars: individual (NY Serpentis) - stars: individual (QW Serpentis) - stars: individual (RX J1155.4-5641) - stars: individual (RZ Leonis) - stars: individual (RZ Sagittae) - stars: individual (TU Crateris) - stars: individual (V2051 Ophiuchi) - stars: individual (WX Ceti) - stars: individual

Simbad objects: 26

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Number of rows : 26
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 V* LL And CV* 00 41 51.4929791640 +26 37 21.043803756           ~ 67 0
2 V* GX Cas CV* 00 49 01.5023646216 +56 52 43.590068220           ~ 39 0
3 V* WX Cet CV* 01 17 04.1794193856 -17 56 22.414606224           ~ 173 0
4 V* KV And CV* 02 17 13.9016014378 +40 41 29.665114908           ~ 29 0
5 V* XZ Eri CV* 04 11 25.7623081800 -15 23 23.764734528           ~ 60 0
6 V* CU Vel CV* 08 58 33.0342318672 -41 47 51.733120236           ~ 109 0
7 PG 0911-066 CV* 09 14 14.0293028112 -06 47 44.773184220   17.6   19.1   ~ 45 0
8 V* KS UMa CV* 10 20 26.5185297792 +53 04 33.089641968   17.0       ~ 75 0
9 V* TU Crt CV* 11 03 36.5725455912 -21 37 45.658609680           ~ 33 0
10 V* RZ Leo CV* 11 37 22.2524330304 +01 48 58.617459936     19.6     DA+dM2 170 0
11 V* BC UMa CV* 11 52 15.8342499696 +49 14 41.887768632           DC: 112 0
12 V* V1040 Cen CV* 11 55 27.2600164728 -56 41 56.294089440           ~ 36 0
13 V* V359 Cen CV* 11 58 15.3250465728 -41 46 08.547000168           DQ: 34 0
14 V* HV Vir CV* 13 21 03.1661521320 +01 53 29.075499492           DA 162 0
15 V* HS Vir CV* 13 43 38.4377401320 -08 14 03.882750324           ~ 61 0
16 V* KV Dra CV* 14 50 38.3283335160 +64 03 29.003633136           DQ 38 0
17 V* NY Ser CV* 15 13 02.2954585632 +23 15 08.407860084   15.648 15.699     ~ 81 0
18 V* QW Ser CV* 15 26 13.9668843408 +08 18 02.490457464           DA:H: 49 0
19 V* V2051 Oph CV* 17 08 19.0873634976 -25 48 31.704262776   17.5       ~ 252 0
20 V* DM Lyr CV* 18 58 44.4381051744 +30 15 33.389060383           ~ 36 0
21 V* RZ Sge CV* 20 03 18.47616 +17 02 51.9432   17.6   17.2   ~ 89 0
22 V* WZ Sge CV* 20 07 36.5037622512 +17 42 14.733254952   15.30 15.20 10.817   D 982 0
23 V* KK Tel CV* 20 28 38.5099147224 -52 18 45.184064220   19.0   19.1   ~ 47 0
24 V* HO Del CV* 20 36 55.4812015512 +14 03 09.406220472           ~ 35 0
25 V* AO Oct CV* 21 05 08.1778533822 -75 21 03.305008201           ~ 28 0
26 V* EI Psc CV* 23 29 54.2146447848 +06 28 11.596023228   16.86 16.22     ~ 141 0

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