The 2003-2004 multisite photometric campaign for the β cephei and eclipsing star 16 (EN) lacertae with an appendix on 2 Andromedae, the variable comparison star

M. Jerzykiewicz, G. Handler, J. Daszyńska-Daszkiewicz, A. Pigulski, E. Poretti, E. Rodríguez, P. J. Amado, Z. Kołaczkowski, K. Uytterhoeven, T. N. Dorokhova, N. I. Dorokhov, D. Lorenz, D. Zsuffa, S. L. Kim, P. O. Bourge, B. Acke, J. De Ridder, T. Verhoelst, R. Drummond, A. I. Movchan & 9 others J. A. Lee, M. Stȩślicki, J. Molenda-Zakowicz, R. Garrido, S. H. Kim, G. Michalska, M. Paparó, V. Antoci, C. Aerts

Research output: Contribution to journalArticle

Abstract

A multisite photometric campaign for the β Cephei and eclipsing variable 16 Lacertae is reported. 749 h of high-quality differential photoelectric Strömgren, Johnson and Geneva time series photometry were obtained with 10 telescopes during 185 nights. After removing the pulsation contribution, an attempt was made to solve the resulting eclipse light curve by means of the computer program EBOP. Although a unique solution was not obtained, the range of solutions could be constrained by comparing computed positions of the secondary component in the Hertzsprung-Russell diagram with evolutionary tracks. For three highamplitude pulsation modes, the uvy and the Geneva UBG amplitude ratios are derived and compared with the theoretical ones for spherical-harmonic degrees ℓ ≤ 4. The highest degree, ℓ = 4, is shown to be incompatible with the observations. One mode is found to be radial, one is ℓ = 1, while in the remaining case ℓ = 2 or 3. The present multisite observations are combined with the archival photometry in order to investigate the long-term variation of the amplitudes and phases of the three high-amplitude pulsation modes. The radial mode shows a non-sinusoidal variation on a time-scale of 73 yr. The ℓ = 1 mode is a triplet with unequal frequency spacing, giving rise to two beat-periods, 720.7 d and 29.1 yr. The amplitude and phase of the ℓ = 2 or 3 mode vary on time-scales of 380.5 d and 43 yr. The light variation of 2 And, one of the comparison stars, is discussed in the appendix.

Original languageEnglish
Pages (from-to)724-740
Number of pages17
JournalMonthly Notices of the Royal Astronomical Society
Volume454
Issue number1
DOIs
Publication statusPublished - 2015

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stars
timescale
photometry
spherical harmonics
Hertzsprung-Russell diagram
spacing
diagram
eclipses
time series
software
night
light curve
comparison
synchronism
telescopes
computer programs

Keywords

  • Individual: 16 (EN) Lacertae
  • Individual: 2 Andromedae
  • Stars
  • Stars
  • Stars oscillations
  • Stars: early-type

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

The 2003-2004 multisite photometric campaign for the β cephei and eclipsing star 16 (EN) lacertae with an appendix on 2 Andromedae, the variable comparison star. / Jerzykiewicz, M.; Handler, G.; Daszyńska-Daszkiewicz, J.; Pigulski, A.; Poretti, E.; Rodríguez, E.; Amado, P. J.; Kołaczkowski, Z.; Uytterhoeven, K.; Dorokhova, T. N.; Dorokhov, N. I.; Lorenz, D.; Zsuffa, D.; Kim, S. L.; Bourge, P. O.; Acke, B.; De Ridder, J.; Verhoelst, T.; Drummond, R.; Movchan, A. I.; Lee, J. A.; Stȩślicki, M.; Molenda-Zakowicz, J.; Garrido, R.; Kim, S. H.; Michalska, G.; Paparó, M.; Antoci, V.; Aerts, C.

In: Monthly Notices of the Royal Astronomical Society, Vol. 454, No. 1, 2015, p. 724-740.

Research output: Contribution to journalArticle

Jerzykiewicz, M, Handler, G, Daszyńska-Daszkiewicz, J, Pigulski, A, Poretti, E, Rodríguez, E, Amado, PJ, Kołaczkowski, Z, Uytterhoeven, K, Dorokhova, TN, Dorokhov, NI, Lorenz, D, Zsuffa, D, Kim, SL, Bourge, PO, Acke, B, De Ridder, J, Verhoelst, T, Drummond, R, Movchan, AI, Lee, JA, Stȩślicki, M, Molenda-Zakowicz, J, Garrido, R, Kim, SH, Michalska, G, Paparó, M, Antoci, V & Aerts, C 2015, 'The 2003-2004 multisite photometric campaign for the β cephei and eclipsing star 16 (EN) lacertae with an appendix on 2 Andromedae, the variable comparison star', Monthly Notices of the Royal Astronomical Society, vol. 454, no. 1, pp. 724-740. https://doi.org/10.1093/mnras/stv1958
Jerzykiewicz, M. ; Handler, G. ; Daszyńska-Daszkiewicz, J. ; Pigulski, A. ; Poretti, E. ; Rodríguez, E. ; Amado, P. J. ; Kołaczkowski, Z. ; Uytterhoeven, K. ; Dorokhova, T. N. ; Dorokhov, N. I. ; Lorenz, D. ; Zsuffa, D. ; Kim, S. L. ; Bourge, P. O. ; Acke, B. ; De Ridder, J. ; Verhoelst, T. ; Drummond, R. ; Movchan, A. I. ; Lee, J. A. ; Stȩślicki, M. ; Molenda-Zakowicz, J. ; Garrido, R. ; Kim, S. H. ; Michalska, G. ; Paparó, M. ; Antoci, V. ; Aerts, C. / The 2003-2004 multisite photometric campaign for the β cephei and eclipsing star 16 (EN) lacertae with an appendix on 2 Andromedae, the variable comparison star. In: Monthly Notices of the Royal Astronomical Society. 2015 ; Vol. 454, No. 1. pp. 724-740.
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abstract = "A multisite photometric campaign for the β Cephei and eclipsing variable 16 Lacertae is reported. 749 h of high-quality differential photoelectric Str{\"o}mgren, Johnson and Geneva time series photometry were obtained with 10 telescopes during 185 nights. After removing the pulsation contribution, an attempt was made to solve the resulting eclipse light curve by means of the computer program EBOP. Although a unique solution was not obtained, the range of solutions could be constrained by comparing computed positions of the secondary component in the Hertzsprung-Russell diagram with evolutionary tracks. For three highamplitude pulsation modes, the uvy and the Geneva UBG amplitude ratios are derived and compared with the theoretical ones for spherical-harmonic degrees ℓ ≤ 4. The highest degree, ℓ = 4, is shown to be incompatible with the observations. One mode is found to be radial, one is ℓ = 1, while in the remaining case ℓ = 2 or 3. The present multisite observations are combined with the archival photometry in order to investigate the long-term variation of the amplitudes and phases of the three high-amplitude pulsation modes. The radial mode shows a non-sinusoidal variation on a time-scale of 73 yr. The ℓ = 1 mode is a triplet with unequal frequency spacing, giving rise to two beat-periods, 720.7 d and 29.1 yr. The amplitude and phase of the ℓ = 2 or 3 mode vary on time-scales of 380.5 d and 43 yr. The light variation of 2 And, one of the comparison stars, is discussed in the appendix.",
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AU - Jerzykiewicz, M.

AU - Handler, G.

AU - Daszyńska-Daszkiewicz, J.

AU - Pigulski, A.

AU - Poretti, E.

AU - Rodríguez, E.

AU - Amado, P. J.

AU - Kołaczkowski, Z.

AU - Uytterhoeven, K.

AU - Dorokhova, T. N.

AU - Dorokhov, N. I.

AU - Lorenz, D.

AU - Zsuffa, D.

AU - Kim, S. L.

AU - Bourge, P. O.

AU - Acke, B.

AU - De Ridder, J.

AU - Verhoelst, T.

AU - Drummond, R.

AU - Movchan, A. I.

AU - Lee, J. A.

AU - Stȩślicki, M.

AU - Molenda-Zakowicz, J.

AU - Garrido, R.

AU - Kim, S. H.

AU - Michalska, G.

AU - Paparó, M.

AU - Antoci, V.

AU - Aerts, C.

PY - 2015

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N2 - A multisite photometric campaign for the β Cephei and eclipsing variable 16 Lacertae is reported. 749 h of high-quality differential photoelectric Strömgren, Johnson and Geneva time series photometry were obtained with 10 telescopes during 185 nights. After removing the pulsation contribution, an attempt was made to solve the resulting eclipse light curve by means of the computer program EBOP. Although a unique solution was not obtained, the range of solutions could be constrained by comparing computed positions of the secondary component in the Hertzsprung-Russell diagram with evolutionary tracks. For three highamplitude pulsation modes, the uvy and the Geneva UBG amplitude ratios are derived and compared with the theoretical ones for spherical-harmonic degrees ℓ ≤ 4. The highest degree, ℓ = 4, is shown to be incompatible with the observations. One mode is found to be radial, one is ℓ = 1, while in the remaining case ℓ = 2 or 3. The present multisite observations are combined with the archival photometry in order to investigate the long-term variation of the amplitudes and phases of the three high-amplitude pulsation modes. The radial mode shows a non-sinusoidal variation on a time-scale of 73 yr. The ℓ = 1 mode is a triplet with unequal frequency spacing, giving rise to two beat-periods, 720.7 d and 29.1 yr. The amplitude and phase of the ℓ = 2 or 3 mode vary on time-scales of 380.5 d and 43 yr. The light variation of 2 And, one of the comparison stars, is discussed in the appendix.

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KW - Individual: 16 (EN) Lacertae

KW - Individual: 2 Andromedae

KW - Stars

KW - Stars

KW - Stars oscillations

KW - Stars: early-type

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