Advertisement

Evidence for Pulsation-Driven Mass Loss from δ Cephei

  • M. Marengo
  • N. R. Evans
  • L. D. Matthews
  • G. Bono
  • P. Barmby
  • D. L. Welch
  • M. Romaniello
  • K. Y. L. Su
  • G. G. Fazio
  • D. Huelsman
Chapter
Part of the Astrophysics and Space Science Proceedings book series (ASSSP, volume 31)

Abstract

We found the first direct evidence that the Cepheid class namesake, δ Cephei, is currently losing mass. These observations are based on data obtained with the Spitzer Space Telescope in the infrared, and with the Very Large Array in the radio. We found that δ Cephei is associated with a vast circumstellar structure, reminiscent of a bow shock. This structure is created as the wind from the star interacts with the local interstellar medium. We measure an outflow velocity of ≈ 35. 5 km s− 1 and a mass loss rate of ≈ 10− 7–10− 6 M year− 1. The very low dust content of the outflow suggests that the wind is possibly pulsation-driven, rather than dust-driven as common for other classes of evolved stars.

Keywords

Stellar Wind Outflow Velocity Instability Strip Mass Loss Process Cepheid Class 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

References

  1. 1.
    Barmby, P., Marengo, M., Evans, N.R., et al.: AJ 141, 42 (2010)ADSCrossRefGoogle Scholar
  2. 2.
    Bono, G., Caputo, F., Castellani, V.: Mem. S. A. It. 77, 207 (2006)ADSGoogle Scholar
  3. 3.
    Caputo, F., Bono, G., Fiorentino, G., et al.: ApJ 629, 1021 (2005)ADSCrossRefGoogle Scholar
  4. 4.
    Cox, A.N.: ARA&A 18, 15 (1980)ADSCrossRefGoogle Scholar
  5. 5.
    Deasy, H.P.: MNRAS 231, 673 (1988)ADSGoogle Scholar
  6. 6.
    Freedman, W.L., Madore, B.F., Scowcroft, W., et al.: AJ 142, 192 (2012)ADSCrossRefGoogle Scholar
  7. 7.
    Gallenne, A., Mérand, A., Kervella, P., Girard, J.H.: A&A 527, 51 (2011)ADSCrossRefGoogle Scholar
  8. 8.
    Kervella, P., Mérand, A., Gallenne, A.: A&A 498, 425 (2011)ADSCrossRefGoogle Scholar
  9. 9.
    Leavitt, H.S.: An. Harv. Coll. Obs., 60, 87 (1908)ADSGoogle Scholar
  10. 10.
    Matthews, L.D., Marengo, M., Evans, N,R., Bono, G.: ApJ 744, 53 (2012)Google Scholar
  11. 11.
    Marengo, M., Evans, N.R., Barmby, P., et al.: ApJ 725, 2392 (2010)ADSCrossRefGoogle Scholar
  12. 12.
    Marengo, M., Sasselov, D.D., Karovska, M., et al.: ApJ 567, 1131 (2002)ADSCrossRefGoogle Scholar
  13. 13.
    McAlary, C.W., Welch, D.L.: AJ 91, 1209 (1986)ADSCrossRefGoogle Scholar
  14. 14.
    Merand, A., Aufdenberg, J.P., Kervella, P., et al.: ApJ 664, 1093 (2007)ADSCrossRefGoogle Scholar
  15. 15.
    Neilson, H.R., Cantiello, M., Langer, N.: A&A 529, L9 (2011)ADSCrossRefGoogle Scholar
  16. 16.
    Neilson, H.R., Ngeow, C-C., Kanbur, S.M., Lester, J.B.: ApJ 692, 81 (2009)Google Scholar

Copyright information

© Springer-Verlag Berlin Heidelberg 2013

Authors and Affiliations

  • M. Marengo
    • 1
  • N. R. Evans
  • L. D. Matthews
  • G. Bono
  • P. Barmby
  • D. L. Welch
  • M. Romaniello
  • K. Y. L. Su
  • G. G. Fazio
  • D. Huelsman
  1. 1.Department of PhysicsIowa State UniversityAmesUSA

Personalised recommendations