2003ApJ...594..961M

Query : 2003ApJ...594..961M

2003ApJ...594..961M - Astrophys. J., 594, 961-970 (2003/September-2)

Constraining the evolution of ZZ Ceti.

MUKADAM A.S., KEPLER S.O., WINGET D.E., NATHER R.E., KILIC M., MULLALLY F., VON HIPPEL T., KLEINMAN S.J., NITTA A., GUZIK J.A., BRADLEY P.A., MATTHEWS J., SEKIGUCHI K., SULLIVAN D.J., SULLIVAN T., SHOBBROOK R.R., BIRCH P., JIANG X.J., XU D.W., JOSHI S., ASHOKA B.N., IBBETSON P., LEIBOWITZ E., OFEK E.O., MEISTAS E.G., JANULIS R., ALISAUSKAS D., KALYTIS R., HANDLER G., KILKENNY D., O'DONOGHUE D., KURTZ D.W., MULLER M., MOSKALIK P., OGLOZA W., ZOLA S., KRZESINSKI J., JOHANNESSEN F., GONZALEZ-PEREZ J.M., SOLHEIM J.-E., SILVOTTI R., BERNABEI S., VAUCLAIR G., DOLEZ N., FU J.N., CHEVRETON M., MANTEIGA M., SUAREZ O., ULLA A., CUNHA M.S., METCALFE T.S., KANAAN A., FRAGA L., COSTA A.F.M., GIOVANNINI O., FONTAINE G., BERGERON P., O'BRIEN M.S., SANWAL D., WOOD M.A., AHRENS T.J., SILVESTRI N., KLUMPE E.W., KAWALER S.D., RIDDLE R., REED M.D. and WATSON T.K.

Abstract (from CDS):

We report our analysis of the stability of pulsation periods in the DAV star (pulsating hydrogen atmosphere white dwarf) ZZ Ceti, also called R548. On the basis of observations that span 31 years, we conclude that the period 213.13 s observed in ZZ Ceti drifts at a rate dP/dt≤(5.5±1.9)x10–15s/s, after correcting for proper motion. Our results are consistent with previous P{dot} values for this mode and an improvement over them because of the larger time base. The characteristic stability timescale implied for the pulsation period is {mid}P/P{dot}{mid}≥1.2 Gyr, comparable to the theoretical cooling timescale for the star. Our current stability limit for the period 213.13 s is only slightly less than the present measurement for another DAV, G117-B15A, for the period 215.2 s, establishing this mode in ZZ Ceti as the second most stable optical clock known, comparable to atomic clocks and more stable than most pulsars. Constraining the cooling rate of ZZ Ceti aids theoretical evolutionary models and white dwarf cosmochronology. The drift rate of this clock is small enough that we can set interesting limits on reflex motion due to planetary companions.

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Journal keyword(s): Stars: Evolution - stars: individual: ZZ Ceti, R548 - Stars: Oscillations - Stars: Variables: Other - Stars: White Dwarfs

CDS comments: Parag. 8 : PSR B1885+09 is a misprint for PSR B1855+09

Simbad objects: 6

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Number of rows : 6
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* ZZ Cet WD* 01 36 13.6153974672 -11 20 32.632874601   14.328 14.16 14.4   DA4.0 307 0
2 V* RY LMi WD* 09 24 15.2482279632 +35 16 51.401570556   15.72   15.99   DA4 274 0
3 V* GW Vir WD* 12 01 45.9731868264 -03 45 40.628670300   14.87 15.04     DOQZ1 505 0
4 V* MY Aps WD* 14 33 07.6366196272 -81 20 14.128475593   13.49 13.35 13.65   DA4.1 152 0
5 V* DN Dra WD* 16 48 25.6318375106 +59 03 22.658985521   12.34 12.17 12.44   DA4.0 228 0
6 PSR B1855+09 Psr 18 57 36.390620 +09 43 17.20712           DA 569 1

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