EDP Sciences
Free Access
Issue
A&A
Volume 578, June 2015
Article Number A101
Number of page(s) 25
Section Stellar atmospheres
DOI https://doi.org/10.1051/0004-6361/201525687
Published online 11 June 2015

Online material

Movie of Fig. 6

Appendix A: Doppler images for the seasons 2007/08 to 2011/12

Appendix A.1: Season 2007/08

In Fig. A.1 five almost consecutive Doppler images are shown, which cover around eight rotations. In Fig. A.2 the spot-model fits of the Doppler images are shown.

thumbnail Fig. A.1

Doppler images of XX Tri for the observing season 2007/08. Each DI is shown in four spherical projections separated by 90°. The rotational shift between consecutive images is corrected, i.e., the stellar orientation remains the same from map to map and from season to season. The time difference between each Doppler image is indicated in units of rotational phase φ.

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thumbnail Fig. A.2

Spot-model fits of the Doppler images in Fig. A.1. Each spot is shown with different color/contrast for better visualization.

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Appendix A.2: Season 2008/09

In Fig. A.3 seven almost consecutive Doppler images are shown, which cover around nine rotations. In Fig. A.4 the spot-model fits of the Doppler images are shown.

thumbnail Fig. A.3

Doppler images of XX Tri for the observing season 2008/09. Otherwise as in Fig. A.1.

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thumbnail Fig. A.4

Spot-model fits of the Doppler images in Fig. A.3. Otherwise as in Fig. A.2.

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Appendix A.3: Season 2009/10

In Fig. A.5 five almost consecutive Doppler images are shown, which cover around eight rotations. In Fig. A.6 the spot-model fits of the Doppler images are shown.

thumbnail Fig. A.5

Doppler images of XX Tri for the observing season 2009/10. Otherwise as in Fig. A.1.

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thumbnail Fig. A.6

Spot-model fits of the Doppler images in Fig. A.5. Otherwise as in Fig. A.2.

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Appendix A.4: Season 2010/11

In Fig. A.7 five almost consecutive Doppler images are shown, which cover around nine rotations. In Fig. A.8 the spot-model fits of the Doppler images are shown.

thumbnail Fig. A.7

Doppler images of XX Tri for the observing season 2010/11. Otherwise as in Fig. A.1.

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thumbnail Fig. A.8

Spot-model fits of the Doppler images in Fig. A.7. Otherwise as in Fig. A.2.

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Appendix A.5: Season 2011/12

In Fig. A.9 seven almost consecutive Doppler images are shown, which cover around ten rotations. In Fig. A.10 the spot-model fits of the Doppler images are shown.

thumbnail Fig. A.9

Doppler images of XX Tri for the observing season 2011/12. Otherwise as in Fig. A.1.

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thumbnail Fig. A.10

Spot-model fits of the Doppler images in Fig. A.9. Otherwise as in Fig. A.2.

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Appendix B: Line profiles of Doppler images for the seasons 2006/07 to 2011/12

Figures B.1 and B.2 show the observed and inverted line profiles of each Doppler image for all observational seasons.

thumbnail Fig. B.1

Line profiles of Doppler images #1–18. Each figure shows the observed (solid lines) and inverted (dotted lines) line profiles for one Doppler image stating their mid times and the respective phases. Rotation advances from bottom to the top. Their corresponding rms-errors are given in Table 3.

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thumbnail Fig. B.2

Line profiles of Doppler images #19-36. Otherwise as in Fig. B.1.

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Appendix C: Phase coverage of Doppler images for the seasons 2006/07 to 2011/12

Figure C.1 shows the phase coverage of each Doppler image for all observational seasons.

thumbnail Fig. C.1

Phase coverage of Doppler images from 2006 to 2012. Different filled (colored) symbols represents the phases of each individual Doppler image, whereas not-filled circles represents non-used spectra (except for gap filling). The arrows indicate the spectra, which were used to fill up large observational gaps. Detailed information is given in Table 3.

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Appendix D: CCF-maps and DR-fits for the seasons 2006/07 to 2011/12

Figure D.1 shows the ccf maps from each observing season. In Fig. D.2 the observed differential rotation pattern determined from the ccf maps, together with the best fit of the differential rotation following Eqs. (5) and (6) are shown.

thumbnail Fig. D.1

Cross-correlation function maps from 2006 to 2012. Each map represents the average ccf map for one observing season.

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thumbnail Fig. D.2

Differential rotation signatures from 2006 to 2012. Analyzing the ccf maps in Fig. D.1 reveals a weak solar-like differential rotation. The dots are the correlation peaks per -latitude bin and their error bars are defined as the FWHMs of the corresponding Gaussians. The dashed line represents a fit using Eq. (5), whereas the solid line represents a fit using Eq. (6). The parameters for each fit are summarized in Table 5.

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Appendix E: Longitudinal spot distribution for the seasons 2006/07 to 2011/12

Figure E.1 shows the mean distribution of the spot area from our spot-model fits for each observing season.

thumbnail Fig. E.1

Longitudinal spot area distribution on XX Tri from 2006 to 2012. Shown are the seasonal mean distributions of the individual spots (solid colored lines) from our spot-model fits for each observing season. The black dashed line represents the total spotted area. The spot area is given in solar hemispheres on the left axis (1 SH=3.05 Gm2) and relative to the total area of a stellar hemisphere of XX Tri on the right axis.

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