DOCSLIB.ORG

Asteroseismology Notes

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Asteroseismology Notes 2 observed pulsations • operate on the dynamical time scale Asteroseismology • accessible on convenient time scale • probe global and local structure Steve Kawaler • periods change on ‘evolutionary’ time scale Iowa State University (thermal or nuclear) - depend on global properties • amplitudes change on ~ ‘local’ thermal time scale 3 4 dynamical stability a more complex example: a star • “stable” configuration represents a stable mean configuration • multiple oscillation modes • on short time scale, oscillations occur, but the • radial modes - enumerated by number of mean value is fixed on longer time scales nodes between center and surface • simple example: a pendulum (single mode) • most likely position - extrema • non-radial modes - nodes also across • mean position is at zero displacement surface of constant radius with no damping would oscillate forever • • modes frequencies determined by solution of • more complex example: a vibrating string the appropriate wave equation • multiple modes with different frequencies • enumerated by number of nodes 5 6 stability, damping, and driving Okay, start your engines... • PG 1159: light curve • zero energy change: what kind of star might this be? constant amplitude oscillation • • what kind of star can this not possibly be? • energy loss via pulsation: • what about the amplitude over the run? oscillation amplitude drops with time • PG 1336 light curve • if net energy input: • huh? what time scale(s) are involved amplitude increases with time • what kind of star (or stars)? (if properly phased) • tell us everything you can about this! 7 8 Multimode pulsation towards the wave equation I Oscillations at “normal mode” frequencies • continuity equation: • @M r =4⇡r2⇢ • mode = specific eigensolution of equations @r of motion within the confines of a stellar • equation of motion (HSE when RHS=0): structure 2 @ r GMr 2 @P 2 = 2 4⇡r • normal mode frequencies parallel structural @t − r − @Mr properties perturb r, P, and ρ: • δx(t, M ) x(t, M )=x (M ) 1+ r simple example: radial fundamental is one r o r x (M ) • o r mode, 1st overtone (a node within) is • and assume δx << x so we can linearize another mode 9 10 towards the wave equation II towards the wave equation III replace x with x+δx in the two equations, • assume adiabatic relationship between P and ρ • @ ln P δP ⇢ subtract off the equilibrium equations, and Γ = so = Γ 1 @ ln ⇢ P 1 ⇢ keep only 1st-order terms to find: ✓ ◆ad o o • combine continuity and equation of motion: linearized continuity equation 2 • @ ⌘ 1 @ 4 @⌘ 1 @ = Γ1Pr + ⌘ [(3Γ1 4) P ] ⇢ δr @(δr/ro) @t2 ⇢r4 @r @r r⇢ @r − = 3 ro ✓ ◆ ⇢ ⇢o − ro − @ro • linearized equation of motion • assume exponential (complex) time dependence 2 d δr/ro δr δP @Po @(δP/Po) δr(t, ro) δr(ro) iσt iσt ⇢oro = 4 + Po = e = ⌘(ro)e dt2 − r P @r − @r ro ro ✓ o o ◆ o o towards the wave equation IV 11 the LAWE: a simple case 12 substitute to yield the Linear Adiabatic Wave • • assume Γ1 and η both constant throughout Equation (LAWE): the star (homologous motion) 1 @ @⌘ 1 @ L(⌘)= Γ Pr4 ⌘ [(3Γ 4) P ] = σ2⌘ LAWE becomes −⇢r4 @r 1 @r − r⇢ @r 1 − • ✓ ◆ ⇢ 1 @P ⌘ (3Γ 4) = σ2⌘ − ⇢r 1 − @r • This is a wave equation: L(η) = σ2η in the • now, assume a constant density, and use HSE displacement η. to replace the pressure derivative to find • the eigenvalue σ2 corresponds to the 2⇡ p⇡ oscillation frequency ⇧ = = σ G⇢¯ (Γ 4 ) 1 − 3 • look familiar?! q 13 14 the LAWE: standing wave solutions the LAWE: asymptotic solution d2w(r) σ2 + φ(r) w(r)=0 boundary conditions: dr2 c2 − • s η represent the eigenfunction as: w(r) eikr r • center: zero displacement ( = 0) • / where kr is the (local) radial wavenumber and surface: perfect wave reflection [d(δP/P)/dr = 0] • varies slowly with radius so, locally: 2 • asymptotic analysis: 2 σ kr = 2 φ(r) • clever change of variables renders LAWE as: cs(r) − d2w(r) σ2⇢ for a standing wave, we need an integral + φ(r) w(r)=0 • dr2 Γ P − number of half-wavelengths between inner 1 • recognizing the sound speed when we see it: and outer reflection points: b d2w(r) σ2 + φ(r) w(r)=0 kr dr =(n + 1)⇡ dr2 c2 − a s Z 15 16 the LAWE: asymptotic solution Nonradial oscillations b 2 2 σ preserve angular derivatives in LAWE kr dr =(n + 1)⇡ where k = φ(r) • r c2(r) − Za s • similar operator structure for radial part (as σ2 before), now along with angular part if φ then • c2 1 2 s b − d δr P 0 Γ1P dr = + 0 + A δr σ =(n + 1)⇡ =(n + 1) σ dt2 r ⇢ ⇢ r · c o ✓ ◆ "Za s # where the quantity A is: d ln ⇢ 1 d ln P 1 χT i.e. high-frequency (high overtone, n) radial A = = [ ad] • dr − Γ1 dr λP χ⇢ rr modes are equally spaced in frequency, with A < 0 when radiative A > 0 when convective σo2 ≈ G<ρ> (the ‘Schwarzschild A’) 17 Spherical Harmonics.... Decompose into Spherical Harmonics courtesy asteroseismology.org (Travis Metcafe) • position perturbation decomposition l=1, m=0 l=1, m=1 δr = δr er + r✓ e✓ + r sin ✓φ eφ • produces (after some work): i=70 2 1 @(r δr) 1 2 2 P 0 δr = r L + 0 r · r2 @r − σ2 ⇢ ✓ ◆ where the operator L2 (the Legendrian) is: l=3, m=0 l=3, m=1 l=3, m=3 1 @ @ 1 @2 L2 = sin ✓ −sin ✓ @✓ @✓ − sin2 ✓ @2 ✓ ◆ • which has eigenstates Ylm such that: 2 m m L Yl (✓, φ)=l(l + 1)Yl (✓, φ) 19 20 using Spherical Harmonics the two characteristic frequencies now we have so: • • 2 2 2 d⌘r l(l + 1) σ 1 @(r δr) l(l + 1) P 0 r = g 2r ⌘r + l(l + 1) 1 r⌘t δr = + 0 dr S2 − − S2 r · r2 @r − σ2r2 ⇢ l l ✓ ◆ 2 2 d⌘t N 2 r expanding into components: r = 1 r⌘r + N 1 r⌘t frequency-2 dr − σ2 g − • 2 2 2 d⌘r gr 2 l(l + 1) σ r 1 where we’ve defined 2 “structural” frequencies r = 2 r⌘r + r 1 r⌘t • dr c2 − r2 − c2 l(l + 1) s s • the acoustic (Lamb) frequency Sl : d⌘ Ag r 2 t 2 l(l + 1) 2 r = 1+ r⌘r + ( Ag) 1 r⌘t S = c dr σ2 − g − l r2 s 2 another frequency • the Brunt-Väisälä (buoyancy) frequency N: d ln ⇢ 1 d ln P N 2 = Ag = g − − dr − Γ dr 1 page 21 22 Propagation diagram, ZAMS solar model NRP dispersion relation • identify the horizontal wave number(s) Sl2, l=1 2 2 l(l + 1) Sl kt = 2 = 2 CZ r cs base • allows the wave equation(s) to reduce to a N2 local dispersion relation, as with the radial case, to provide relationship between kr and σ: 2 1 2 2 2 2 kr = 2 2 (σ N )(σ Sl ) σ cs − − 23 page 24 asymptotic analysis Propagation diagram, ZAMS solar model 2 1 2 2 2 2 kr = 2 2 (σ N )(σ Sl ) σ cs − − Sl2, l=1 2 • kr > 0 (kr real) when l=1 n=4 CZ l=1 n=3 • σ2 > N2, Sl2 - or - σ2 < N2, Sl2 base l=1 n=2 l=1 n=1 • kr real means oscillatory eigenfunctions N2 • kr2 < 0 (kr imaginary) when • Sl2 > σ2 > N2 or Sl2 < σ2 < N2 • kr real means evanescent (exponentially decreasing or increasing) eigenfunctions page 25 page 26 Propagation diagram, ZAMS solar model Propagation diagram, ZAMS solar model “high” σ oscillatory evanescent evanescent zones 2 2 zones Sl , l=1 zones Sl , l=1 in pink in gray in gray l=1 n=4 l=1 n=4 CZ l=1 n=3 CZ l=1 n=3 base l=1 n=2 base l=1 n=2 l=1 n=1 l=1 n=1 N2 N2 “low” σ oscillatory zones in green 27 page 28 the NRP LAWE: asymptotic solutions Propagation diagram, ZAMS solar model “high” σ • again, integrate dispersion relation over oscillatory evanescent zones propagation regions: zones 2 b Sl , l=1 in pink 2 1 2 2 2 2 in gray kr dr =(n + 1)⇡ where k = (σ N )(σ S ) r σ2c2 − − l l=1 n=4 Za s CZ l=1 n=3 • two classes of solutions: base l=1 n=2 b l=1 n=1 2 2 2 dr • σ > N , Sl : σnl =(n + l/2)σo ; σo = 2 l=1 n=1 a cs N “p-modes”; pressure as the restoring forceZ l=1 n=2 • l=1 n=3 l=1 n=4 1 b − 2 2 2 ⇧o 2 N “low” σ σ < N , Sl : ⇧nl = n ; ⇧o =2⇡ dr • l(l + 1) r "Za # oscillatory “g-modes”: buoyancy as the restoring force • p zones in green page 29 page Pulsation Periods Period of ‘radial fundamental’ ~ tff g-modes p-modes Π > t Π < t Periods ff ff restoring force buoyancy pressure asymptotic Π ∝ Π x n σ ∝ σ x n behavior o o Cepheids, white dwarfs examples the Sun 31 Solar Oscillations: Full-disk photometry p. 32 p-modes: ~ equally spaced in frequency Frohlich et al. 1997: SOHO/VIRGO 10 5 1 hr min min b dr σ =(n + l/2)σ ; σ = nl o o c Za s l l l l l l l l l n-2 n-1 n n+1 n+2 n+3 n+4 n+5 n+6 ... ... frequency l+1 l+1 l+1 l+1 l+1 l+1 l+1 l+1 n-2 n-1 n n+1 n+2 n+3 n+4 n+5 • if modes of different l present, observed 20 parts per million! spacing ~ σo / 2 Solar Oscillations: Full-disk photometry p.
Load more

Recommended publications
  • Characterizing Two Solar-Type Kepler Subgiants with Asteroseismology: Kic 10920273 and Kic 11395018
    The Astrophysical Journal, 763:49 (10pp), 2013 January 20 doi:10.1088/0004-637X/763/1/49 C 2013. The American Astronomical Society. All rights reserved. Printed in the U.S.A. CHARACTERIZING TWO SOLAR-TYPE KEPLER SUBGIANTS WITH ASTEROSEISMOLOGY: KIC 10920273 AND KIC 11395018 G. Doganˇ 1,2,3, T. S. Metcalfe1,3,4, S. Deheuvels3,5,M.P.DiMauro6, P. Eggenberger7, O. L. Creevey8,9,10, M. J. P. F. G. Monteiro11, M. Pinsonneault3,12, A. Frasca13, C. Karoff2, S. Mathur1,S.G.Sousa11,I.M.Brandao˜ 11, T. L. Campante11,14, R. Handberg2, A. O. Thygesen2,15, K. Biazzo16,H.Bruntt2, E. Niemczura17, T. R. Bedding18, W. J. Chaplin3,14, J. Christensen-Dalsgaard2,3,R.A.Garc´ıa3,19, J. Molenda-Zakowicz˙ 17, D. Stello18, J. L. Van Saders3,12, H. Kjeldsen2, M. Still20, S. E. Thompson21, and J. Van Cleve21 1 High Altitude Observatory, National Center for Atmospheric Research, P.O. Box 3000, Boulder, CO 80307, USA; [email protected] 2 Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark 3 Kavli Institute for Theoretical Physics, Kohn Hall, University of California, Santa Barbara, CA 93106, USA 4 Space Science Institute, Boulder, CO 80301, USA 5 Department of Astronomy, Yale University, P.O. Box 208101, New Haven, CT 06520-8101, USA 6 INAF-IAPS, Istituto di Astrofisica e Planetologia Spaziali, Via del Fosso del Cavaliere 100, I-00133 Roma, Italy 7 Geneva Observatory, University of Geneva, Maillettes 51, 1290 Sauverny, Switzerland 8 Universite´ de Nice, Laboratoire Cassiopee,´ CNRS UMR 6202, Observatoire de la Coteˆ d’Azur, BP 4229, F-06304 Nice Cedex 4, France 9 IAC Instituto de Astrof´ısica de Canarias, C/V´ıa Lactea´ s/n, E-38200 Tenerife, Spain 10 Universidad de La Laguna, Avda.
    [Show full text]
  • Magnetism, Dynamo Action and the Solar-Stellar Connection
    Living Rev. Sol. Phys. (2017) 14:4 DOI 10.1007/s41116-017-0007-8 REVIEW ARTICLE Magnetism, dynamo action and the solar-stellar connection Allan Sacha Brun1 · Matthew K. Browning2 Received: 23 August 2016 / Accepted: 28 July 2017 © The Author(s) 2017. This article is an open access publication Abstract The Sun and other stars are magnetic: magnetism pervades their interiors and affects their evolution in a variety of ways. In the Sun, both the fields themselves and their influence on other phenomena can be uncovered in exquisite detail, but these observations sample only a moment in a single star’s life. By turning to observa- tions of other stars, and to theory and simulation, we may infer other aspects of the magnetism—e.g., its dependence on stellar age, mass, or rotation rate—that would be invisible from close study of the Sun alone. Here, we review observations and theory of magnetism in the Sun and other stars, with a partial focus on the “Solar-stellar connec- tion”: i.e., ways in which studies of other stars have influenced our understanding of the Sun and vice versa. We briefly review techniques by which magnetic fields can be measured (or their presence otherwise inferred) in stars, and then highlight some key observational findings uncovered by such measurements, focusing (in many cases) on those that offer particularly direct constraints on theories of how the fields are built and maintained. We turn then to a discussion of how the fields arise in different objects: first, we summarize some essential elements of convection and dynamo theory, includ- ing a very brief discussion of mean-field theory and related concepts.
    [Show full text]
  • Planet Hunters1 (Fischer Et Al
    draft version May 31, 2012 Planet Hunters: Assessing the Kepler Inventory of Short Period Planets Megan E. Schwamb1,2,3,Chris J. Lintott4,5, Debra A. Fischer6, Matthew J. Giguere6, Stuart Lynn5,4, Arfon M. Smith5,4, John M. Brewer6, Michael Parrish5, Kevin Schawinski2,3,7, and Robert J. Simpson4 [email protected] ABSTRACT We present the results from a search of data from the first 33.5 days of the Kepler science mission (Quarter 1) for exoplanet transits by the Planet Hunters citizen science project. Planet Hunters enlists members of the general public to visually identify tran- sits in the publicly released Kepler light curves via the World Wide Web. Over 24,000 volunteers reviewed the Kepler Quarter 1 data set. We examine the abundance of ≥ 2 R⊕ planets on short period (< 15 days) orbits based on Planet Hunters detections. We present these results along with an analysis of the detection efficiency of human classifiers to identify planetary transits including a comparison to the Kepler inventory of planet candidates. Although performance drops rapidly for smaller radii, ≥ 4 R⊕ Planet Hunters ≥ 85% efficient at identifying transit signals for planets with periods less than 15 days for the Kepler sample of target stars. Our high efficiency rate for simulated transits along with recovery of the majority of Kepler ≥4R⊕ planets suggest suggests the Kepler inventory of ≥4 R⊕ short period planets is nearly complete. Subject headings: Planets and satellites: detection-Planets and satellites: general 1. Introduction In the past nearly two decades, there has been an explosion in the number of known planets arXiv:1205.6769v1 [astro-ph.EP] 30 May 2012 orbiting stars beyond our own solar system, with over 700 extrasolar planets (exoplanets) known 1Yale Center for Astronomy and Astrophysics, Yale University,P.O.
    [Show full text]
  • 20 Jun 2012 Kepler-36: a Pair of Planets with Neighboring Orbits
    Kepler-36: A Pair of Planets with Neighboring Orbits and Dissimilar Densities Joshua A. Carter1+∗, Eric Agol2+∗, William J. Chaplin3, Sarbani Basu4, Timothy R. Bedding5, Lars A. Buchhave6, Jørgen Christensen-Dalsgaard7, Katherine M. Deck8, Yvonne Elsworth3, Daniel C. Fabrycky9, Eric B. Ford10, Jonathan J. Fortney11, Steven J. Hale3, Rasmus Handberg7, Saskia Hekker12, Matthew J. Holman13, Daniel Huber14, Christopher Karoff7, Steven D. Kawaler15, Hans Kjeldsen7, Jack J. Lissauer14, Eric D. Lopez11, Mikkel N. Lund7, Mia Lundkvist7, Travis S. Metcalfe16, Andrea Miglio3, Leslie A. Rogers8, Dennis Stello5, William J. Borucki14, Steve Bryson14, Jessie L. Christiansen17, William D. Cochran18, John C. Geary13, Ronald L. Gilliland19, Michael R. Haas14, Jennifer Hall20, Andrew W. Howard21, Jon M. Jenkins17, Todd Klaus20, David G. Koch14, David W. Latham13, Phillip J. MacQueen18, Dimitar Sasselov13, Jason H. Steffen22, Joseph D. Twicken17, Joshua N. Winn8 1Hubble Fellow, Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 2Department of Astronomy, Box 351580, University of Washington, Seattle, WA 98195, USA arXiv:1206.4718v1 [astro-ph.EP] 20 Jun 2012 3School of Physics and Astronomy, University of Birmingham, Edgbaston, B15 2TT, UK 4Department and Astronomy, Yale University, New Haven, CT, 06520, USA 5Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, Australia Niels Bohr Institute, Copenhagen University, DK-2100 Copenhagen, Denmark 6Centre for Star and Planet Formation, Natural History
    [Show full text]
  • Development of a Stellar Model-Fitting Pipeline for Asteroseismic Data from the TESS Mission
    Development of a Stellar Model-Fitting Pipeline for Asteroseismic Data from the TESS Mission PI: Travis Metcalfe / Co-I: Rich Townsend Collaborators: David Guenther, Dennis Stello The launch of NASA’s Kepler space telescope in 2009 revolutionized the quality and quantity of observational data available for asteroseismic analysis. Prior to the Kepler mission, solar-like oscillations were extremely difficult to observe, and data only existed for a handful of the brightest stars in the sky. With the necessity of studying one star at a time, the traditional approach to extracting the physical properties of the star from the observations was an uncomfortably subjective process. A variety of experts could use similar tools but come up with significantly different answers. Not only did this subjectivity have the potential to undermine the credibility of the technique, it also hindered the compilation of a uniform sample that could be used to draw broader physical conclusions from the ensemble of results. During a previous award from NASA, we addressed these issues by developing an automated and objective stellar model-fitting pipeline for Kepler data, and making it available through the Asteroseismic Modeling Portal (AMP). This community modeling tool has allowed us to derive reliable asteroseismic radii, masses and ages for large samples of stars (Metcalfe et al., 2014), but the most recent observations are so precise that we are now limited by systematic uncertainties associated with our stellar models. With a huge archive of Kepler data available for model validation, and the next planet-hunting satellite already approved for an expected launch in 2017, now is the time to incorporate what we have learned into the next generation of AMP.
    [Show full text]
  • IAU Symp 269, POST MEETING REPORTS
    IAU Symp 269, POST MEETING REPORTS C.Barbieri, University of Padua, Italy Content (i) a copy of the final scientific program, listing invited review speakers and session chairs; (ii) a list of participants, including their distribution on gender (iii) a list of recipients of IAU grants, stating amount, country, and gender; (iv) receipts signed by the recipients of IAU Grants (done); (v) a report to the IAU EC summarizing the scientific highlights of the meeting (1-2 pages). (vi) a form for "Women in Astronomy" statistics. (i) Final program Conference: Galileo's Medicean Moons: their Impact on 400 years of Discovery (IAU Symposium 269) Padova, Jan 6-9, 201 Program Wednesday 6, location: Centro San Gaetano, via Altinate 16.0 0 – 18.00 meeting of Scientific Committee (last details on the Symp 269; information on the IYA closing ceremony program) 18.00 – 20.00 welcome reception Thursday 7, morning: Aula Magna University 8:30 – late registrations 09.00 – 09.30 Welcome Addresses (Rector of University, President of COSPAR, Representative of ESA, President of IAU, Mayor of Padova, Barbieri) Session 1, The discovery of the Medicean Moons, the history, the influence on human sciences Chair: R. Williams Speaker Title 09.30 – 09.55 (1) G. Coyne Galileo's telescopic observations: the marvel and meaning of discovery 09.55 – 10.20 (2) D. Sobel Popular Perceptions of Galileo 10.20 – 10.45 (3) T. Owen The slow growth of human humility (read by Scott Bolton) 10.45 – 11.10 (4) G. Peruzzi A new Physics to support the Copernican system. Gleanings from Galileo's works 11.10 – 11.35 Coffee break Session 1b Chair: T.
    [Show full text]
  • Curriculum Vitae Michael John Thompson
    Curriculum Vitae Michael John Thompson Michael J. Thompson, MA, PhD, FRAS Interim President, University Corporation for Atmospheric Research, Boulder, CO, USA Deputy Director and Chief Operating Officer, National Center for Atmospheric Research, Boulder, CO, USA Contact Details Work tel: +1 303 497 1652 E-mail: [email protected] Web: https://president.ucar.edu/ Home address: 5840 Flagstaff Road, Boulder, CO 80302, USA Home tel: +1 303 443 3816 Postgraduate Employment 2010 { National Center for Atmospheric Research (NCAR), and University Corporation for Atmospheric Research (UCAR) Interim UCAR President (2015 { ) NCAR Deputy Director, and Chief Operating Officer (2013 { ) NCAR Associate Director (2010 { 2013) Director of the High Altitude Observatory (2010 { 2014) NCAR Senior Scientist (2010 { ) 2004 { 2015 University of Sheffield Professor of Applied Mathematics & Solar Physics Head of School of Mathematics & Statistics (2007 { 2010) Chair of School of Mathematics & Statistics (2005 { 2007) Head of Department of Applied Mathematics (2004 { 2007) 2001 { 2004 Imperial College London Professor of Physics Deputy Head of the Space & Atmospheric Physics Group (2003 { 2004) 1990 { 2000 Queen Mary, University of London Reader in Mathematics and Astronomy (1996 { 2000) Lecturer in Astronomy (1990 { 1996) SERC Postdoctoral Fellow (1990 { 1992) 1990 Institute for Theoretical Physics, Univ. California Santa Barbara Post-doctoral researcher 1988 { 1989 High Altitude Observatory, Boulder CO, USA Visiting scientist 1987 { 1988 Institute for Astronomy, Aarhus University, Denmark Post-doctoral researcher 1981 { 1983 Pafec Ltd., Nottingham, U.K. Management trainee Academic qualifications PhD (1988; University of Cambridge); MA (1985; University of Cambridge); Cert. Advanced Studies in Mathematics, with distinction (1984; University of Cambridge); BA Hons (1981; University of Cambridge).
    [Show full text]
  • Kepler Mission Stellar and Instrument Noise Properties
    University of Birmingham Kepler Mission stellar and instrument noise properties Gilliland, Ronald L.; Chaplin, William J.; Dunham, Edward W.; Argabright, Vic S.; Borucki, William J.; Basri, Gibor; Bryson, Stephen T.; Buzasi, Derek L.; Caldwell, Douglas A.; Elsworth, Yvonne P.; Jenkins, Jon M.; Koch, David G.; Kolodziejczak, Jeffrey; Miglio, Andrea; Van Cleve, Jeffrey; Walkowicz, Lucianne M.; Welsh, William F. DOI: 10.1088/0067-0049/197/1/6 License: None: All rights reserved Document Version Publisher's PDF, also known as Version of record Citation for published version (Harvard): Gilliland, RL, Chaplin, WJ, Dunham, EW, Argabright, VS, Borucki, WJ, Basri, G, Bryson, ST, Buzasi, DL, Caldwell, DA, Elsworth, YP, Jenkins, JM, Koch, DG, Kolodziejczak, J, Miglio, A, Van Cleve, J, Walkowicz, LM & Welsh, WF 2011, 'Kepler Mission stellar and instrument noise properties', Astrophysical Journal. Supplement Series, vol. 197, no. 1, 6. https://doi.org/10.1088/0067-0049/197/1/6 Link to publication on Research at Birmingham portal Publisher Rights Statement: © American Astronomical Society. Published in The Astrophysical Journal Supplement Series - http://iopscience.iop.org/0067-0049/197/1/6/. Eligibility for repository checked August 2014. General rights Unless a licence is specified above, all rights (including copyright and moral rights) in this document are retained by the authors and/or the copyright holders. The express permission of the copyright holder must be obtained for any use of this material other than for purposes permitted by law. •Users may freely distribute the URL that is used to identify this publication. •Users may download and/or print one copy of the publication from the University of Birmingham research portal for the purpose of private study or non-commercial research.
    [Show full text]
  • Asteroseismology of Solar-Type Stars with Kepler I: Data Analysis C
    Asteroseismology of solar-type stars with Kepler I: Data analysis C. Karoff, W.J. Chaplin, Thierry Appourchaux, Y. Elsworth, R.A. Garcia, G. Houdek, T.S. Metcalfe, J. Molenda-Żakowicz, M.J.P.F.G. Monteiro, M.J. Thompson, et al. To cite this version: C. Karoff, W.J. Chaplin, Thierry Appourchaux, Y. Elsworth, R.A. Garcia, et al.. Asteroseismology of solar-type stars with Kepler I: Data analysis. Astronomical Notes / Astronomische Nachrichten, Wiley-VCH Verlag, 2010, 331 (9-10), pp.972-976. 10.1002/asna.201011438. hal-00683333 HAL Id: hal-00683333 https://hal.archives-ouvertes.fr/hal-00683333 Submitted on 18 Oct 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Astron. Nachr. / AN 331, No. 9/10, 972 – 976 (2010) / DOI 10.1002/asna.201011438 Asteroseismology of solar-type stars with Kepler I: Data analysis C. Karoff1,2,, W.J. Chaplin1, T. Appourchaux3,Y.Elsworth1,R.A.Garcia4, G. Houdek5, T.S. Metcalfe6, J. Molenda-Zakowicz˙ 7, M.J.P.F.G. Monteiro8, M.J. Thompson9, J. Christensen- Dalsgaard2, R.L. Gilliland10,H.Kjeldsen2,S.Basu11, T.R. Bedding12, T.L. Campante2,8, P.
    [Show full text]
  • Asteroseismic Analysis of 15 Solar-Like Oscillating Evolved Stars
    MNRAS 000, 1–10 (0000) Preprint 12 May 2021 Compiled using MNRAS LATEX style file v3.0 Asteroseismic analysis of 15 solar-like oscillating evolved stars Z. ¸Celik Orhan,1⋆ M. Yıldız 1 and C. Kayhan1,2 1Department of Astronomy and Space Sciences, Science Faculty, Ege University, 35100, Bornova, Izmir,˙ Turkey 2Department of Astronomy and Space Sciences, Science Faculty, Erciyes University, 38030, Melikgazi, Kayseri, Turkey Accepted XXX. Received YYY; in original form ZZZ ABSTRACT Asteroseismology using space-based telescopes is vital to our understanding of stellar structure and evolution. CoRoT , Kepler, and TESS space telescopes have detected large numbers of solar-like oscillating evolved stars. Solar-like oscillation frequencies have an important role in the determination of fundamental stellar parameters; in the literature, the relations between the two is established by the so-called scaling relations. In this study, we analyse data obtained from the observation of 15 evolved solar-like oscillating stars using the Kepler and ground-based telescopes. The main purpose of the study is to determine very precisely the fundamental parameters of evolved stars by constructing interior models using asteroseismic parameters. We also fit the reference frequencies of models to the observational reference frequencies caused by the He II ionization zone. The 15 evolved stars are found to have masses and radii within ranges of 0.79-1.47 M⊙ and 1.60-3.15 R⊙, respectively. Their model ages range from 2.19to 12.75 Gyr. It is revealed that fitting reference frequencies typically increase the accuracy of asteroseismic radius, mass, and age. The typical uncertainties of mass and radius are ∼ 3-6 and ∼ 1-2 per cent, respectively.
    [Show full text]
  • Asteroseismology of Solar-Type Stars
    Living Reviews in Solar Physics (2019) 16:4 https://doi.org/10.1007/s41116-019-0020-1 REVIEW ARTICLE Asteroseismology of solar-type stars Rafael A. García1,2 · Jérôme Ballot3 Received: 29 August 2018 / Accepted: 19 June 2019 / Published online: 9 September 2019 © The Author(s) 2019 Abstract Until the last few decades, investigations of stellar interiors had been restricted to theoretical studies only constrained by observations of their global properties and external characteristics. However, in the last 30years the field has been revolutionized by the ability to perform seismic investigations of stellar interiors. This revolution begun with the Sun, where helioseismology has been yielding information competing with what can be inferred about the Earth’s interior from geoseismology. The last two decades have witnessed the advent of asteroseismology of solar-like stars, thanks to a dramatic development of new observing facilities providing the first reliable results on the interiors of distant stars. The coming years will see a huge development in this field. In this review we focus on solar-type stars, i.e., cool main-sequence stars where oscillations are stochastically excited by surface convection. After a short introduction and a historical overview of the discipline, we review the observational techniques generally used, and we describe the theory behind stellar oscillations in cool main- sequence stars. We continue with a complete description of the normal mode analyses through which it is possible to extract the physical information about the structure and dynamics of the stars. We then summarize the lessons that we have learned and discuss unsolved issues and questions that are still unanswered.
    [Show full text]
  • Bibliography from ADS File: Chaplin.Bib May 31, 2021 1
    Bibliography from ADS file: chaplin.bib Metcalfe, T. S., van Saders, J. L., Basu, S., et al., “The Evolution of Rota- August 16, 2021 tion and Magnetic Activity in 94 Aqr Aa from Asteroseismology with TESS”, 2020ApJ...900..154M ADS Nielsen, M. B., Ball, W. H., Standing, M. R., et al., “TESS asteroseismology of Zinn, J. C., Stello, D., Elsworth, Y., et al., “The K2 Galactic Archaeology the known planet host star λ2 Fornacis”, 2020A&A...641A..25N ADS Program Data Release 3: Age-abundance patterns in C1-C8, C10-C18”, Steinmetz, M., Guiglion, G., McMillan, P. J., et al., “The Sixth Data Release of 2021arXiv210805455Z ADS the Radial Velocity Experiment (RAVE). II. Stellar Atmospheric Parameters, Lyttle, A. J., Davies, G. R., Li, T., et al., “Hierarchically modelling Kepler Chemical Abundances, and Distances”, 2020AJ....160...83S ADS dwarfs and subgiants to improve inference of stellar properties with astero- Steinmetz, M., Matijevic,ˇ G., Enke, H., et al., “The Sixth Data Release of the Ra- seismology”, 2021MNRAS.505.2427L ADS dial Velocity Experiment (RAVE). I. Survey Description, Spectra, and Radial Hill, M. L., Kane, S. R., Campante, T. L., et al., “Asteroseismology of Velocities”, 2020AJ....160...82S ADS iota Draconis and Discovery of an Additional Long-Period Companion”, Ahumada, R., Prieto, C. A., Almeida, A., et al., “The 16th Data Release of 2021arXiv210713583H ADS the Sloan Digital Sky Surveys: First Release from the APOGEE-2 Southern Thomas, A. E. L., Chaplin, W. J., Basu, S., et al., “Impact of magnetic Survey and Full Release of eBOSS Spectra”, 2020ApJS..249....3A ADS activity on inferred stellar properties of main-sequence Sun-like stars”, Jiang, C., Bedding, T.
    [Show full text]