Constraining the evolution of ZZ Ceti

Anjum S. Mukadam; S. O. Kepler; D. E. Winget; R. E. Nather; M. Kilic; F. Mullally; T. Von Hippel; S. J. Kleinman; A. Nitta; J. A. Guzik; P. A. Bradley; J. Matthews; K. Sekiguchi; D. J. Sullivan; T. Sullivan; R. R. Shobbrook; P. Birch; X. J. Jiang; D. W. Xu; S. Joshi; B. N. Ashoka; P. Ibbetson; E. Leibowitz; E. O. Ofek; E. G. Meištas; R. Janulis; D. Ališauskas; R. Kalytis; G. Handler; D. Kilkenny; D. O'Donoghue; D. W. Kurtz; M. Müller; P. Moskalik; W. Ogłoza; S. Zoła; J. Krzesiński; F. Johannessen; J. M. Gonzalez-Perez; J. E. Solheim; R. Silvotti; S. Bernabei; G. Vauclair; N. Dolez; J. N. Fu; M. Chevreton; M. Manteiga; O. Suárez; A. Ulla; M. S. Cunha; T. S. Metcalfe; A. Kanaan; L. Fraga; A. F.M. Costa; O. Giovannini; G. Fontaine; P. Bergeron; M. S. O'Brien; D. Sanwal; M. A. Wood; T. J. Ahrens; N. Silvestri; E. W. Klumpe; S. D. Kawaler; R. Riddle; M. D. Reed; T. K. Watson

doi:10.1086/377044

Constraining the evolution of ZZ Ceti

Anjum S. Mukadam^*, S. O. Kepler, D. E. Winget, R. E. Nather, M. Kilic, F. Mullally, T. Von Hippel, S. J. Kleinman, A. Nitta, J. A. Guzik, P. A. Bradley, J. Matthews, K. Sekiguchi, D. J. Sullivan, T. Sullivan, R. R. Shobbrook, P. Birch, X. J. Jiang, D. W. Xu, S. JoshiB. N. Ashoka, P. Ibbetson, E. Leibowitz, E. O. Ofek, E. G. Meištas, R. Janulis, D. Ališauskas, R. Kalytis, G. Handler, D. Kilkenny, D. O'Donoghue, D. W. Kurtz, M. Müller, P. Moskalik, W. Ogłoza, S. Zoła, J. Krzesiński, F. Johannessen, J. M. Gonzalez-Perez, J. E. Solheim, R. Silvotti, S. Bernabei, G. Vauclair, N. Dolez, J. N. Fu, M. Chevreton, M. Manteiga, O. Suárez, A. Ulla, M. S. Cunha, T. S. Metcalfe, A. Kanaan, L. Fraga, A. F.M. Costa, O. Giovannini, G. Fontaine, P. Bergeron, M. S. O'Brien, D. Sanwal, M. A. Wood, T. J. Ahrens, N. Silvestri, E. W. Klumpe, S. D. Kawaler, R. Riddle, M. D. Reed, T. K. Watson

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

36 Citations (Scopus)

Abstract

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) × 10^-15 s s^-1, after correcting for proper motion. Our results are consistent with previous Ṗ 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 | Ṗ / |≥ 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.

Original language	English
Pages (from-to)	961-970
Number of pages	10
Journal	Astrophysical Journal
Volume	594
Issue number	2 I
DOIs	https://doi.org/10.1086/377044
Publication status	Published - 10 Sept 2003

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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., ... Watson, T. K. (2003). Constraining the evolution of ZZ Ceti. Astrophysical Journal, 594(2 I), 961-970. https://doi.org/10.1086/377044

@article{0dd5df43d057455a86641452a9c0d344,

title = "Constraining the evolution of ZZ Ceti",

abstract = "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) × 10-15 s s-1, after correcting for proper motion. Our results are consistent with previous Ṗ 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 | Ṗ / |≥ 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.",

keywords = "Stars: evolution, Stars: individual (ZZ Ceti, R548), Stars: oscillations, Stars: variables: other, White dwarfs",

author = "Mukadam, {Anjum S.} and Kepler, {S. O.} and Winget, {D. E.} and Nather, {R. E.} and M. Kilic and F. Mullally and {Von Hippel}, T. and Kleinman, {S. J.} and A. Nitta and Guzik, {J. A.} and Bradley, {P. A.} and J. Matthews and K. Sekiguchi and Sullivan, {D. J.} and T. Sullivan and Shobbrook, {R. R.} and P. Birch and Jiang, {X. J.} and Xu, {D. W.} and S. Joshi and Ashoka, {B. N.} and P. Ibbetson and E. Leibowitz and Ofek, {E. O.} and Mei{\v s}tas, {E. G.} and R. Janulis and D. Ali{\v s}auskas and R. Kalytis and G. Handler and D. Kilkenny and D. O'Donoghue and Kurtz, {D. W.} and M. M{\"u}ller and P. Moskalik and W. Og{\l}oza and S. Zo{\l}a and J. Krzesi{\'n}ski and F. Johannessen and Gonzalez-Perez, {J. M.} and Solheim, {J. E.} and R. Silvotti and S. Bernabei and G. Vauclair and N. Dolez and Fu, {J. N.} and M. Chevreton and M. Manteiga and O. Su{\'a}rez and A. Ulla and Cunha, {M. S.} and Metcalfe, {T. S.} and A. Kanaan and L. Fraga and Costa, {A. F.M.} and O. Giovannini and G. Fontaine and P. Bergeron and O'Brien, {M. S.} and D. Sanwal and Wood, {M. A.} and Ahrens, {T. J.} and N. Silvestri and Klumpe, {E. W.} and Kawaler, {S. D.} and R. Riddle and Reed, {M. D.} and Watson, {T. K.}",

year = "2003",

month = sep,

day = "10",

doi = "10.1086/377044",

language = "English",

volume = "594",

pages = "961--970",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "2 I",

}

Mukadam, AS, Kepler, SO, Winget, DE, Nather, RE, Kilic, M, Mullally, F, Von Hippel, T, Kleinman, SJ, Nitta, A, Guzik, JA, Bradley, PA, Matthews, J, Sekiguchi, K, Sullivan, DJ, Sullivan, T, Shobbrook, RR, Birch, P, Jiang, XJ, Xu, DW, Joshi, S, Ashoka, BN, Ibbetson, P, Leibowitz, E, Ofek, EO, Meištas, EG, Janulis, R, Ališauskas, D, Kalytis, R, Handler, G, Kilkenny, D, O'Donoghue, D, Kurtz, DW, Müller, M, Moskalik, P, Ogłoza, W, Zoła, S, Krzesiński, J, Johannessen, F, Gonzalez-Perez, JM, Solheim, JE, Silvotti, R, Bernabei, S, Vauclair, G, Dolez, N, Fu, JN, Chevreton, M, Manteiga, M, Suárez, O, Ulla, A, Cunha, MS, Metcalfe, TS, Kanaan, A, Fraga, L, Costa, AFM, Giovannini, O, Fontaine, G, Bergeron, P, O'Brien, MS, Sanwal, D, Wood, MA, Ahrens, TJ, Silvestri, N, Klumpe, EW, Kawaler, SD, Riddle, R, Reed, MD & Watson, TK 2003, 'Constraining the evolution of ZZ Ceti', Astrophysical Journal, vol. 594, no. 2 I, pp. 961-970. https://doi.org/10.1086/377044

TY - JOUR

T1 - Constraining the evolution of ZZ Ceti

AU - Mukadam, Anjum S.

AU - Kepler, S. O.

AU - Winget, D. E.

AU - Nather, R. E.

AU - Kilic, M.

AU - Mullally, F.

AU - Von Hippel, T.

AU - Kleinman, S. J.

AU - Nitta, A.

AU - Guzik, J. A.

AU - Bradley, P. A.

AU - Matthews, J.

AU - Sekiguchi, K.

AU - Sullivan, D. J.

AU - Sullivan, T.

AU - Shobbrook, R. R.

AU - Birch, P.

AU - Jiang, X. J.

AU - Xu, D. W.

AU - Joshi, S.

AU - Ashoka, B. N.

AU - Ibbetson, P.

AU - Leibowitz, E.

AU - Ofek, E. O.

AU - Meištas, E. G.

AU - Janulis, R.

AU - Ališauskas, D.

AU - Kalytis, R.

AU - Handler, G.

AU - Kilkenny, D.

AU - O'Donoghue, D.

AU - Kurtz, D. W.

AU - Müller, M.

AU - Moskalik, P.

AU - Ogłoza, W.

AU - Zoła, S.

AU - Krzesiński, J.

AU - Johannessen, F.

AU - Gonzalez-Perez, J. M.

AU - Solheim, J. E.

AU - Silvotti, R.

AU - Bernabei, S.

AU - Vauclair, G.

AU - Dolez, N.

AU - Fu, J. N.

AU - Chevreton, M.

AU - Manteiga, M.

AU - Suárez, O.

AU - Ulla, A.

AU - Cunha, M. S.

AU - Metcalfe, T. S.

AU - Kanaan, A.

AU - Fraga, L.

AU - Costa, A. F.M.

AU - Giovannini, O.

AU - Fontaine, G.

AU - Bergeron, P.

AU - O'Brien, M. S.

AU - Sanwal, D.

AU - Wood, M. A.

AU - Ahrens, T. J.

AU - Silvestri, N.

AU - Klumpe, E. W.

AU - Kawaler, S. D.

AU - Riddle, R.

AU - Reed, M. D.

AU - Watson, T. K.

PY - 2003/9/10

Y1 - 2003/9/10

N2 - 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) × 10-15 s s-1, after correcting for proper motion. Our results are consistent with previous Ṗ 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 | Ṗ / |≥ 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.

AB - 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) × 10-15 s s-1, after correcting for proper motion. Our results are consistent with previous Ṗ 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 | Ṗ / |≥ 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.

KW - Stars: evolution

KW - Stars: individual (ZZ Ceti, R548)

KW - Stars: oscillations

KW - Stars: variables: other

KW - White dwarfs

UR - http://www.scopus.com/inward/record.url?scp=0242508372&partnerID=8YFLogxK

U2 - 10.1086/377044

DO - 10.1086/377044

M3 - Article

SN - 0004-637X

VL - 594

SP - 961

EP - 970

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2 I

ER -

Constraining the evolution of ZZ Ceti

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