Journal
ASTROPHYSICAL JOURNAL
Volume 782, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/782/1/18
Keywords
stars: interiors; stars: oscillations
Categories
Funding
- NASA's Science Mission Directorate
- National Initiative on Undergraduate Science (NIUS) program of HBCSE (TIFR)
- NSF [AST-1105930]
- Austrian Science Fund (FWF) [P21205-N16]
- FCT/MCTES, Portugal [PTDC/CTE-AST/098754/2008]
- POPH/FSE (EC)
- Excellence cluster Origin and Structure of the Universe (Garching)
- CNES
- Danish National Research Foundation
- ASTERISK project (ASTERoseismic Investigations with SONG and Kepler)
- European Research Council [267864]
- National Science Foundation
- NASA [NNX12AE17G]
- European Commission under SPACEINN [FP7-SPACE-2012-312844]
- Science and Technology Facilities Council [ST/J001163/1] Funding Source: researchfish
- STFC [ST/J001163/1] Funding Source: UKRI
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1105930] Funding Source: National Science Foundation
- Austrian Science Fund (FWF) [P21205] Funding Source: Austrian Science Fund (FWF)
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For the very best and brightest asteroseismic solar-type targets observed by Kepler, the frequency precision is sufficient to determine the acoustic depths of the surface convective layer and the helium ionization zone. Such sharp features inside the acoustic cavity of the star, which we call acoustic glitches, create small oscillatory deviations from the uniform spacing of frequencies in a sequence of oscillation modes with the same spherical harmonic degree. We use these oscillatory signals to determine the acoustic locations of such features in 19 solar-type stars observed by the Kepler mission. Four independent groups of researchers utilized the oscillation frequencies themselves, the second differences of the frequencies and the ratio of the small and large separation to locate the base of the convection zone and the second helium ionization zone. Despite the significantly different methods of analysis, good agreement was found between the results of these four groups, barring a few cases. These results also agree reasonably well with the locations of these layers in representative models of the stars. These results firmly establish the presence of the oscillatory signals in the asteroseismic data and the viability of several techniques to determine the location of acoustic glitches inside stars.
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