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Evaluation Projects for Pulsating Stars Jørgen Christensen-Dalsgaard (29 February, 2016)

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Evaluation Projects for Pulsating Stars Jørgen Christensen-Dalsgaard (29 February, 2016) Evaluation projects for Pulsating Stars Jørgen Christensen-Dalsgaard (29 February, 2016) The projects should result in a report of up to around 10 pages, which may be written in Danish or English. Here I expect a description of the general problem considered, and an analysis starting from the references provided, but, as required, taken into account also other references or material. It may be appropriate to present derivations in more detail than provided in the papers. The required papers can in most cases be found through the reprint server ADS, at http://adsabs.harvard.edu/abstract service.html. Also, they are often available as preprints at the arXiv preprint server, at http://xxx.lanl.gov/archive/astro-ph. In some cases, refer- ences are given to papers that may be difficult to find; in that case, I shall lend them to you to copy. A few projects also involve simple numerical analyses or calculations; they can be carried out in any language, but I expect the report to include relevant plots of the results. There should be enough suggestions that you can each get your own project. They will be distributed on a first-come first-served basis. When you have chosen a project I ask you to send me an e-mail ([email protected]) with your name, study number (˚arskortnummer) and the number of the project. I shall keep a list of the project numbers that have already been reserved on the home page of the course. The report should similarly be e-mailed to me, as a PDF file. The reports will be graded according to the 12 scale. In the evaluation, I shall give substantial weight to the appropriate combination of results from several sources and/or independent analysis. 1. Helioseismic effect of revision of solar abundances Although solar models have been found to agree quite well with helioseismic inferences (e.g. Gough et al. 1996), this agreement has been seriously compromised by a recent revision of the solar surface abundances (very recently reviewed by Asplund et al. 2009). These issues were discussed by Basu & Antia (2004), Bahcall et al. (2005) and Christensen-Dalsgaard et al. (2009). Discuss this problem and its possible solution; this should also include a brief review of the relevant analysis techniques, including those presented by Basu & Antia (1997). References: Asplund, M., Grevesse, N., Sauval, A. J. & Scott, P., 2009. [The chemical composition of the Sun]. Annu. Rev. Astron. Astrophys., 47, 481 { 522. Bahcall, J. N., Basu, S., Pinsonneault, M. & Serenelli, A. M., 2005. [Helioseismological implications of recent solar abundance determinations]. Astrophys. J., 618, 1049 { 1056. Basu, S. & Antia, H. M., 1997. [Seismic measurement of the depth of the solar convection zone]. Mon. Not. R. astr. Soc., 287, 189 { 198. Basu, S. & Antia, H. M., 2004. [Constraining solar abundances using helioseismology]. Astrophys. J., 606, L85 { L88. Christensen-Dalsgaard, J., Di Mauro, M. P., Houdek, G. & Pijpers, F., 2009. [On the opacity change required to compensate for the revised solar composition]. Astron. Astrophys., 494, 205 { 208. Gough, D. O., Kosovichev, A. G., Toomre, J., et al., 1996. [The seismic structure of the Sun]. Science, 272, 1296 { 1300. 1 2. Asteroseismic analysis of main-sequence stars based on Kepler data The Kepler mission has provided detailed frequency spectra for a substantial number of main- sequence stars, and we are just at the beginning of learning how to analyse them in the best possible way. This also involves extensive comparisons of computations using different evolution codes. Based on the examples in the following references discuss what has been learned so far, and how these analyses can be extended and improved. You may include, and possibly criticize, the review provided by Christensen-Dalsgaard (2012). References: Christensen-Dalsgaard, J., 2012. [Stellar model fits and inversions]. Astron. Nachr., 333, 914 { 925. Mathur, S., Metcalfe, T. S., Woitaszek, M., et al., 2012. [A uniform asteroseismic analysis of 22 solar-type stars observed by Kepler]. Astrophys. J., 749, 152-(1 { 14). Metcalfe, T. S., Chaplin, W. J., Appourchaux, T., et al., 2012. [Asteroseismology of the solar analogs 16 Cyg A and B from Kepler observations]. Astrophys. J., 748, L10-(1 { 6). Metcalfe, T. S., Creevey, L. O. & Davies, G. R., 2015. [Asteroseismic modeling of 16 Cyg A & B using the complete Kepler data set]. Astrophys. J., 811, L37-(1 { 5). Silva Aguirre, V., Basu, S., Brand~ao,I. M., et al., 2013. [Stellar ages and convective cores in field main-sequence stars: first asteroseismic application to two Kepler targets]. Astrophys. J., 769, 141-(1 { 17). 3. Asteroseismic characterization of exoplanet host stars Asteroseismology based on Kepler data provides a unique possibility for determining the proper- ties stars found by the mission to host extra-solar planets, essentially from the same photometric observations. In particular, the stellar radius and mass are needed to determine radii and masses of the exoplanets, while asteroseismology also provides the possibility to determine the age of the star and its planetary system. The following references give some examples of this type of analysis. You should discuss the potential and the possible problems in determining the stellar properties and the importance for characterizing the exoplanets. You may also find other examples of this type of analysis in the literature. References: Christensen-Dalsgaard, J., Kjeldsen, H., Brown, T. M., Gilliland, R. L., Arentoft, T., Frandsen, S., Quirion, P.-O., Borucki, W. J., Koch, D. & Jenkins, J. M., 2010. [Asteroseismic investigation of known planet hosts in the Kepler field]. Astrophys. J., 713, L164 { L168. Fogtmann-Schulz, A., Hinrup, B., Van Eylen, V., Christensen-Dalsgaard, J., Kjeldsen, H., Silva Aguirre, V. & Tingley, B., 2014. [Accurate parameters of the oldest known rocky-exoplanet hosting system: Kepler-10 revisited]. Astrophys. J., 781, 67-(1 { 8). Silva Aguirre, V., Davies, G. R., Basu, S., et al., 2015. [Ages and fundamental properties of Kepler exoplanet host stars from asteroseismology]. Mon. Not. R. astr. Soc., 452, 2127 { 2148. 2 4. A detailed example of asteroseismic model fitting Lebreton & Goupil (2014) gave a very detailed and illustrative analysis of a star observed by the CoRoT mission, comparing the results of using different combinations of asteroseismic and `classical' constraints. Also, the provided extensive tables of additional properties of the models, allowing further investigations of how these properties are related and constrained by the data. In this project you should discuss the analysis in the paper and try to carry it further by using the data provided in connection with the paper. I hope that this can provide additional insight for you (and me!) on how the properties of the models depend on the assumed physics etc. References: Lebreton, Y. & Goupil, M. J., 2014. [Asteroseismology for “`ala carte" stellar age-dating and weighing. Age and mass of the CoRoT exoplanet host HD 52265]. Astron. Astrophys., 569, A21-(1 { 24). 5. Asteroseismic analysis of the α Centauri system Solar-like oscillations have been detected in both main components of the α Cen binary system. The masses of these components span the solar mass; furthermore, the properties of the stars are known with unusually good precision due to their proximity, and from analysis of the binary motion. Thus the system provides excellent opportunities for asteroseismology. The references discuss observations of the system and attempts at analysing the results. In the project, discuss the observational data and the modelling, and the conclusions reached so far. What will be required to improve both observations and models? References: Bedding, T. R., Kjeldsen, H., Butler, R. P., McCarthy, C., Marcy, G. W., O'Toole, S. J., Tinney, C. G. & Wright, J. T., 2004. [Oscillation frequencies and mode lifetimes in α Centauri A]. Astrophys. J., 614, 380 { 385. Bouchy, F. & Carrier, F., 2002. [The acoustic spectrum of α Cen A]. Astron. Astrophys., 390, 205 { 212. Carrier, F. & Bourban, G., 2003. [Solar-like oscillations in the K1 dwarf star α Cen B]. Astron. Astrophys., 406, L23 { L26. de Meulenaer, P., Carrier, F., Miglio, A., Bedding, T. R., Campante, T. L., Eggenberger, P., Kjeldsen, H. & Montalb´an,J., 2010. [Core properties of α Centauri A using asteroseismology]. Astron. Astrophys., 523, A54-(1 { 8). Eggenberger, P., Charbonnel, C., Talon, S., Meynet, G., Maeder, A., Carrier, F. & Bourban, G., 2004. [Analysis of α Centauri AB including seismic constraints]. Astron. Astrophys., 417, 235 { 246. Kjeldsen, H., Bedding, T. R., Butler, R. P., Christensen-Dalsgaard, J., Kiss, L. L., McCarthy, C., Marcy, G. W., Tinney, C. G. & Wright, J. T., 2005. [Solar-like oscillations in α Centauri B]. Astrophys. J., 635, 1281 { 1290. Miglio, A. & Montalb´an,J., 2005. [Constraining fundamental stellar parameters using seismology. Application to α Centauri AB]. Astron. Astrophys., 441, 615 { 629. 3 6. Asteroseismic diagnostics of subgiant stars Subgiants, i.e., stars in the hydrogen shell-burning phase evolving towards the red-giant branch, are very interesting from an asteroseismic point of view. They typically show mixed modes, with great diagnostic potential, and they have somewhat larger amplitudes, owing to their larger luminosity, than stars on the main sequence. Here we consider examples of asteroseismic diagnostics of such stars based on CoRoT and Kepler observations. References: Metcalfe, T. S., Monteiro, M. J. P. F. G., Thompson, M. J., et al., 2010. [A precise asteroseismic age and radius for the evolved Sun-like star KIC 11026764]. Astrophys. J., 723, 1583 { 1598. Deheuvels, S. & Michel, E., 2011. [Constraints on the structure of the core of subgiants via mixed modes: the case of HD 49385]. Astron. Astrophys., 535, A91-(1 { 19). Di Mauro, M. P., Cardini, D., Catanzaro, G., et al., 2011. [Solar-like oscillations from the depths of the red-giant star KIC 4351319 observed with Kepler]. Mon.
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