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Title: The occurrence of non-pulsating stars in the γ Dor and δ Sct pulsation instability regions: Results from Kepler quarter 14–17 data

Journal Article · · Astronomical Review
 [1];  [1];  [2];  [3];  [4];  [5]
  1. Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
  2. New Mexico State Univ., Las Cruces, NM (United States)
  3. New Mexico State Univ., Las Cruces, NM (United States); Uniwersytet Wroclawski, Wroclaw (Poland)
  4. Instituto de Astrofisica de Canarias(IAC), La Laguna (Spain); Univ. de La Laguna, La Laguna (Spain)
  5. Apache Point Observatory, Sunspot, NM (United States)
+ Show Author Affiliations

In this study, the high precision long time-series photometry of the NASA Kepler spacecraft provides an excellent means to discover and characterize variability in main-sequence stars, and to make progress in interpreting the pulsations to derive stellar interior structure and test stellar models. For stars of spectral types A–F, the Kepler data revealed a number of surprises, such as more hybrid pulsating Sct and Dor pulsators than expected, pulsators lying outside of the instability regions predicted by theory, and stars that were expected to pulsate, but showed no variability. In our 2013 Astronomical Review article, we discussed the statistics of variability for 633 faint (Kepler magnitude 14–16) spectral type A–F stars observed by Kepler during Quarters 6–13 (June 2010–June 2012).

Research Organization:
Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)
Sponsoring Organization:
USDOE
Grant/Contract Number:
AC52-06NA25396
OSTI ID:
1234653
Report Number(s):
LA-UR-14-29153
Journal Information:
Astronomical Review, Vol. 11, Issue 1; ISSN 2167-2857
Country of Publication:
United States
Language:
English

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Cited By (1)

Candidates for non-pulsating stars located in the Cepheid instability strip in the Large Magellanic Cloud based on Strömgren photometry journal August 2019

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79 ASTRONOMY AND ASTROPHYSICS
variable stars
stellar pulsation
Kepler spacecraft