Surface magnetic activity of the fast-rotating G5 giant in Comae, central star of the faint planetary nebula LoTr 5

Z. Kővári, K. G. Strassmeier, K. Oláh, L. Kriskovics, K. Vida, T. A. Carroll, T. Granzer, I. Ilyin, J. Jurcsik, E. Kovári, M. Weber

Research output: Contribution to journalArticle

Abstract

Context. On the asymptotic giant branch, low to intermediate mass stars blow away their outer envelopes, forming planetary nebulae. Dynamic interaction between the planetary nebula and its central progenitor is poorly understood. The interaction is even more complex when the central object is a binary star with a magnetically active component, as is the case for the target in this paper. Aims. We aim to quantify the stellar surface activity of the cool binary component of IN Com and aim to explain its origin. In general, we need a better understanding of how central binary stars in planetary nebulae evolve and how this evolution could develop such magnetically active stars as IN Com. Methods. We present a time series of 13 consecutive Doppler images covering six months in 2017 that we used to measure the surface differential rotation with a cross-correlation method. Hitherto unpublished high-precision photometric data from 1989 to 2017 are presented. We applied Fourier-transformation-based frequency analysis to both photometry and spectra. Very high resolution (R 200 000) spectra were used to update IN Com's astrophysical parameters by means of spectral synthesis. Results. Our time-series Doppler images show cool and warm spots coexisting with an average surface temperature contrast of -1000 K and +300 K with respect to the effective temperature. Approximately 8% of the stellar surface is covered with cool spots and ~3% with warm spots. A consistent cool polar spot is seen in all images. The average lifetime of the cool spots is not much more than a few stellar rotations (one month), while the warm spots appear to live longer (three months) and are mostly confined to high latitudes. We found anti-solar surface differential rotation with a shear coefficient of α = -0.026 ± 0.005 suggesting an equatorial rotation period of 5.973 ± 0.008 d. We reconfirm the 5.9 day rotation period of the cool star from photometry, radial velocities, and Hα line-profile variations. A long-term V-brightness variation with a likely period of 7.2 yr is also found. It appears in phase with the orbital radial velocity of the binary system in the sense that it is brightest at highest velocity and faintest at lowest velocity, that is, at the two phases of quadrature. We redetermine [Ba/Fe], [Y/Fe], and [Sr/Fe] ratios and confirm the overabundance of these s-process elements in the atmosphere of IN Com.

Original languageEnglish
Article numberA83
JournalAstronomy and Astrophysics
Volume624
DOIs
Publication statusPublished - Apr 1 2019

Fingerprint

planetary nebulae
stars
binary stars
radial velocity
photometry
orbital velocity
H lines
stellar rotation
cool stars
time series
Fourier transformation
quadratures
polar regions
cross correlation
surface temperature
low speed
frequency analysis
astrophysics
brightness
coverings

Keywords

  • Stars: activity
  • Stars: imaging
  • Stars: individual: IN Com
  • Stars: late-type
  • Starspots

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Surface magnetic activity of the fast-rotating G5 giant in Comae, central star of the faint planetary nebula LoTr 5. / Kővári, Z.; Strassmeier, K. G.; Oláh, K.; Kriskovics, L.; Vida, K.; Carroll, T. A.; Granzer, T.; Ilyin, I.; Jurcsik, J.; Kovári, E.; Weber, M.

In: Astronomy and Astrophysics, Vol. 624, A83, 01.04.2019.

Research output: Contribution to journalArticle

Kővári, Z. ; Strassmeier, K. G. ; Oláh, K. ; Kriskovics, L. ; Vida, K. ; Carroll, T. A. ; Granzer, T. ; Ilyin, I. ; Jurcsik, J. ; Kovári, E. ; Weber, M. / Surface magnetic activity of the fast-rotating G5 giant in Comae, central star of the faint planetary nebula LoTr 5. In: Astronomy and Astrophysics. 2019 ; Vol. 624.
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abstract = "Context. On the asymptotic giant branch, low to intermediate mass stars blow away their outer envelopes, forming planetary nebulae. Dynamic interaction between the planetary nebula and its central progenitor is poorly understood. The interaction is even more complex when the central object is a binary star with a magnetically active component, as is the case for the target in this paper. Aims. We aim to quantify the stellar surface activity of the cool binary component of IN Com and aim to explain its origin. In general, we need a better understanding of how central binary stars in planetary nebulae evolve and how this evolution could develop such magnetically active stars as IN Com. Methods. We present a time series of 13 consecutive Doppler images covering six months in 2017 that we used to measure the surface differential rotation with a cross-correlation method. Hitherto unpublished high-precision photometric data from 1989 to 2017 are presented. We applied Fourier-transformation-based frequency analysis to both photometry and spectra. Very high resolution (R 200 000) spectra were used to update IN Com's astrophysical parameters by means of spectral synthesis. Results. Our time-series Doppler images show cool and warm spots coexisting with an average surface temperature contrast of -1000 K and +300 K with respect to the effective temperature. Approximately 8{\%} of the stellar surface is covered with cool spots and ~3{\%} with warm spots. A consistent cool polar spot is seen in all images. The average lifetime of the cool spots is not much more than a few stellar rotations (one month), while the warm spots appear to live longer (three months) and are mostly confined to high latitudes. We found anti-solar surface differential rotation with a shear coefficient of α = -0.026 ± 0.005 suggesting an equatorial rotation period of 5.973 ± 0.008 d. We reconfirm the 5.9 day rotation period of the cool star from photometry, radial velocities, and Hα line-profile variations. A long-term V-brightness variation with a likely period of 7.2 yr is also found. It appears in phase with the orbital radial velocity of the binary system in the sense that it is brightest at highest velocity and faintest at lowest velocity, that is, at the two phases of quadrature. We redetermine [Ba/Fe], [Y/Fe], and [Sr/Fe] ratios and confirm the overabundance of these s-process elements in the atmosphere of IN Com.",
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AU - Strassmeier, K. G.

AU - Oláh, K.

AU - Kriskovics, L.

AU - Vida, K.

AU - Carroll, T. A.

AU - Granzer, T.

AU - Ilyin, I.

AU - Jurcsik, J.

AU - Kovári, E.

AU - Weber, M.

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N2 - Context. On the asymptotic giant branch, low to intermediate mass stars blow away their outer envelopes, forming planetary nebulae. Dynamic interaction between the planetary nebula and its central progenitor is poorly understood. The interaction is even more complex when the central object is a binary star with a magnetically active component, as is the case for the target in this paper. Aims. We aim to quantify the stellar surface activity of the cool binary component of IN Com and aim to explain its origin. In general, we need a better understanding of how central binary stars in planetary nebulae evolve and how this evolution could develop such magnetically active stars as IN Com. Methods. We present a time series of 13 consecutive Doppler images covering six months in 2017 that we used to measure the surface differential rotation with a cross-correlation method. Hitherto unpublished high-precision photometric data from 1989 to 2017 are presented. We applied Fourier-transformation-based frequency analysis to both photometry and spectra. Very high resolution (R 200 000) spectra were used to update IN Com's astrophysical parameters by means of spectral synthesis. Results. Our time-series Doppler images show cool and warm spots coexisting with an average surface temperature contrast of -1000 K and +300 K with respect to the effective temperature. Approximately 8% of the stellar surface is covered with cool spots and ~3% with warm spots. A consistent cool polar spot is seen in all images. The average lifetime of the cool spots is not much more than a few stellar rotations (one month), while the warm spots appear to live longer (three months) and are mostly confined to high latitudes. We found anti-solar surface differential rotation with a shear coefficient of α = -0.026 ± 0.005 suggesting an equatorial rotation period of 5.973 ± 0.008 d. We reconfirm the 5.9 day rotation period of the cool star from photometry, radial velocities, and Hα line-profile variations. A long-term V-brightness variation with a likely period of 7.2 yr is also found. It appears in phase with the orbital radial velocity of the binary system in the sense that it is brightest at highest velocity and faintest at lowest velocity, that is, at the two phases of quadrature. We redetermine [Ba/Fe], [Y/Fe], and [Sr/Fe] ratios and confirm the overabundance of these s-process elements in the atmosphere of IN Com.

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KW - Stars: imaging

KW - Stars: individual: IN Com

KW - Stars: late-type

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