Imaging Spotted RS CVn • Compare aperture synthesis images with contemporaneous Doppler imaging...

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Transcript of Imaging Spotted RS CVn • Compare aperture synthesis images with contemporaneous Doppler imaging...

  • CHARA 2015 Towards Adaptive Optics at CHARA

    Imaging Spotted RS CVn Binaries

    Rachael Roettenbacher University of Michigan

    John Monnier, Fabien Baron, Xiao Che, Ettore Pedretti, Heidi Korhonen, Bob Harmon, Greg Henry, Frank Fekel, Mike Williamson, Dave Latham, and the CHARA Collaboration

  • CHARA 2015 Towards Adaptive Optics at CHARA

    Imaging Spotted Stars with CHARA

    •  Compare aperture synthesis images with contemporaneous Doppler imaging and light-curve inversion results

    •  Interferometry from MIRC 6T •  High-resolution spectroscopy from VLT, NOT,

    STELLA robotic telescope •  Photometry from APT and SMARTS •  RS CVn targets: ζ And and σ Gem

  • CHARA 2015 Towards Adaptive Optics at CHARA

    RS CVn Binaries •  Giant or subgiant primary

    component •  Subgiant or dwarf

    secondary component •  Exhibit photometric and

    Ca H and K variability •  Interesting starspot features

    •  Polar spots •  Active longitudes

    •  Close binaries •  Short rotation and orbital

    periods •  Often tidally-locked •  No mass transfer Hall 1976, Berdyugina 2005, Strassmeier 2009

  • CHARA 2015 Towards Adaptive Optics at CHARA

    o Dra

    370x fainter than primary

    Red Giant Primary Star R1 = 25.2 +\- 0.2 Rsun

    Main sequence companion

    Roettenbacher et al. in prep.

    •  G9III primary •  Teff ~ 4430 K •  Prot ~ 70 days •  Porb ~138 days •  Active primary

    •  Spot evolution •  Ca H & K variation

    •  No direct detections of the companion star

  • CHARA 2015 Towards Adaptive Optics at CHARA

    ο Dra Orbit

    Roettenbacher et al. in prep. 6 4 2 0 -2 -4 -6

    milliarcsecond

    -6

    -4

    -2

    0

    2

    4

    6

    m illi

    ar cs

    ec on

    d

    2012 May 09 2012 May 12

    2012 Jun 17 2012 Jun 18

    2014 May 26 2014 May 27

    o Dra A

    o Dra B

  • CHARA 2015 Towards Adaptive Optics at CHARA

    -0.2 0.0 0.2 0.4 0.6 0.8 1.0 1.2 Phase

    -60

    -40

    -20

    0

    Ve lo

    ci ty

    (k m

    /s )

    -0.2 0.0 0.2 0.4 0.6 0.8 1.0 1.2 Phase

    -20

    0

    20

    40

    60

    80

    100

    R a d ia

    l V e lo

    ci ty

    ( km

    /s )

    Roettenbacher et al. in prep.

    ο Dra Radial Velocity Curve

  • CHARA 2015 Towards Adaptive Optics at CHARA

    8000 7000 6000 5000 4000 Teff (K)

    1

    10

    100

    Bo lo

    m et

    ric L

    um in

    os ity

    (L Su

    n)

    ZAMS 3 Gyr Isochrone Primary Evolutionary

    track(1.36 MSun) with 1- Mass Errors Secondary Evolutionary Track

    (0.99 MSun) with 1- Mass Errors Primary Stellar Parameters with 1- Errors Secondary Stellar Parameters with 1- Errors

    Roettenbacher et al. in prep.

    ο Dra Mass and Evolution

  • CHARA 2015 Towards Adaptive Optics at CHARA

    Roettenbacher et al. in prep.

    ο Dra Ellipsoidal Variations

    0.06 0.04

    0.02

    0.00

    -0.02

    -0.04

    B

    -0.2 0.0 0.2 0.4 0.6 0.8 1.0 1.2 Phase

    0.06 0.04

    0.02

    0.00

    -0.02

    -0.04

    V

    = 0.08 = 0.08 = 0.08 = 0.08 = 0.08 = 0.25 = 0.25 = 0.25 = 0.25 = 0.25

  • CHARA 2015 Towards Adaptive Optics at CHARA

    o Dra

    370x fainter than primary

    Red Giant Primary Star R1 = 25.2 +\- 0.2 Rsun

    Main sequence companion

    Roettenbacher et al. in prep.

    •  t ~ 3 +/- 0.5 Gyr •  M1 = 1.36 +/- 0.04 Msun •  M2 = 0.99 +/- 0.02 Msun •  T1 ~ 4430 +/- 130 K •  T2 ~ 6000 +400/-300 K •  R1 = 25.2 +/- 0.2 Rsun •  R2 = 1.0 +/- 0.1 Rsun •  Active primary?

    •  Ellipsoidal variations •  Eclipsing

  • CHARA 2015 Towards Adaptive Optics at CHARA

    σ Gem

    4 2014 – Submission Deadline: 13 Dec 2013, midnight EST (Friday night)– Submit to proposals@chara-array.org

    J. Science Justification/Figures/Tables (Insert as needed) –

    Figure 1 (left) shows a detection of the binary companion of σ Gem (flux ratio 250:1; 2012 Nov 7). Figure 1 (right) is our orbit fit of σ Gem (red; with parameters given in Dümmler et al. 1997) with σ Gem using our radius (dotted line) and our dates of detection and their locations on the orbit (diamonds).

    Figure 2 (left) shows the detection of the binary companion of ο Dra (flux ratio 350:1; 2012 Jun 18). Figure 2 (right) is in the same sense as Figure 1 (right) for ο Dra (with orbital parameters from D. Latham). The detections of ο Dra are less robust, so request more observations to improve the quality of our binary fit and determine the masses and spectral types of the components. References Dümmler, R., Ilyin, I. V., & Tuominen, I. 1997, A&AS, 123, 209 Habets, G. M. H. J. & Zwaan, C. 1989, A&A, 211, 56 Hall, D. S. & Persinger, W. T. 1986, LNP, 254, 88 Henry, G. W., Eaton, J. A., Hamer, J., & Hall, D. S. 1995, ApJS, 97, 513 Lucy, L. B. & Sweeney, M. A. 1971, AJ, 76, 544 Young, R. K. 1920, PDAO, 1, 263 Zahn, J.-P. 1977, A&A, 57, 383

    270x fainter than primary

    Red Giant Primary Star R1 = 10.1 +\- 0.2 Rsun

    Main-sequence Companion

    Roettenbacher et al. submitted

    •  K1III primary •  Teff ~ 4530 K •  Prot ~ Porb ~19.6 days •  Active primary

    •  Active longitudes •  Spot evolution •  Differential

    rotation •  No direct detections of

    the companion star

  • CHARA 2015 Towards Adaptive Optics at CHARA

    σ Gem Orbit

    Roettenbacher et al. submitted 4 2 0 -2 -4

    milliarcsecond

    -4

    -2

    0

    2

    4 m

    illi ar

    cs ec

    on d

    2011 Dec 08

    2012 Nov 07 2012 Nov 08

    2012 Nov 24

    2012 Nov 25

    Gem A Gem B

  • CHARA 2015 Towards Adaptive Optics at CHARA

    Roettenbacher et al. submitted

    σ Gem Radial Velocity Curve

    -0.2 0.0 0.2 0.4 0.6 0.8 1.0 1.2 Phase

    -20

    0

    20

    40

    60

    80

    100

    R ad

    ia l V

    el oc

    ity (k

    m /s

    )

  • CHARA 2015 Towards Adaptive Optics at CHARA

    Roettenbacher et al. submitted

    σ Gem Mass and Evolution

    7000 6000 5000 4000 3000 Teff (K)

    0.01

    0.10

    1.00

    10.00

    100.00

    Bo lo

    m et

    ric L

    um in

    os ity

    (L Su

    n)

    ZAMS 5 Gyr Isochrone Primary Evolutionary Track (1.28 MSun) with 1- Mass Errors Secondary Evolutionary Track (0.73 MSun) with 1- Mass Errors Primary Stellar Parameters with 1- Errors Secondary Stellar Parameters with 1- Errors

  • CHARA 2015 Towards Adaptive Optics at CHARA

    Roettenbacher et al. submitted

    σ Gem Ellipsoidal Variations

    0.06 0.04

    0.02

    0.00

    -0.02

    -0.04

    B

    -0.2 0.0 0.2 0.4 0.6 0.8 1.0 1.2 Phase

    0.06 0.04

    0.02

    0.00

    -0.02

    -0.04

    V

    = 0.02 = 0.02 = 0.02 = 0.02 = 0.02 = 0.08 = 0.08 = 0.08 = 0.08 = 0.08 = 0.25 = 0.25 = 0.25 = 0.25 = 0.25

  • CHARA 2015 Towards Adaptive Optics at CHARA

    σ Gem

    4 2014 – Submission Deadline: 13 Dec 2013, midnight EST (Friday night)– Submit to proposals@chara-array.org

    J. Science Justification/Figures/Tables (Insert as needed) –

    Figure 1 (left) shows a detection of the binary companion of σ Gem (flux ratio 250:1; 2012 Nov 7). Figure 1 (right) is our orbit fit of σ Gem (red; with parameters given in Dümmler et al. 1997) with σ Gem using our radius (dotted line) and our dates of detection and their locations on the orbit (diamonds).

    Figure 2 (left) shows the detection of the binary companion of ο Dra (flux ratio 350:1; 2012 Jun 18). Figure 2 (right) is in the same sense as Figure 1 (right) for ο Dra (with orbital parameters from D. Latham). The detections of ο Dra are less robust, so request more observations to improve the quality of our binary fit and determine the masses and spectral types of the components. References Dümmler, R., Ilyin, I. V., & Tuominen, I. 1997, A&AS, 123, 209 Habets, G. M. H. J. & Zwaan, C. 1989, A&A, 211, 56 Hall, D. S. & Persinger, W. T. 1986, LNP, 254, 88 Henry, G. W., Eaton, J. A., Hamer, J., & Hall, D. S. 1995, ApJS, 97, 513 Lucy, L. B. & Sweeney, M. A. 1971, AJ, 76, 544 Young, R. K. 1920, PDAO, 1, 263 Zahn, J.-P. 1977, A&A, 57, 383

    270x fainter than primary

    Red Giant Primary Star R1 = 10.1 +\- 0.2 Rsun

    Main-sequence Companion

    Roettenbacher et al. submitted

    •  t ~ 5 +/- 1 Gyr •  M1 = 1.28 +/- 0.07 Msun •  M2 = 0.73 +/- 0.02 Msun •  T1 ~ 4530 +/- 60 K •  T2 ~ 4300 K •  R1 = 10.1 +/- 0.2 Rsun •  R2 ~ 0.7 Rsun •  Active primary

    •  Large starspots •  Ellipsoidal variations

  • CHARA 2015 Towards Adaptive Optics at CHARA

    RS CVn Imaging

    •  Inte