skip to main content
Explore Scholarly Publications and Datasets in the NSF-PAR

  • Home
  • Search Results
  • Page 1 of 2

Search for: All records

Creators/Authors contains: "Caldwell, Douglas A."

Note: When clicking on a Digital Object Identifier (DOI) number, you will be taken to an external site maintained by the publisher. Some full text articles may not yet be available without a charge during the embargo (administrative interval).
What is a DOI Number?

Some links on this page may take you to non-federal websites. Their policies may differ from this site.

  1. ; ; ; ; ; ; ; ; ; ; et al ( , The Astronomical Journal)
    Full Text Available 
  2. ; ; ; ; ; ; ; ; ; ; et al ( , The Astronomical Journal)
    Full Text Available 
  3. ; ; ; ; ; ; ; ; ; ; et al ( , The Astronomical Journal)
    Full Text Available 
  4. ; ; ; ; ; ; ; ; ; ; et al ( , The Astronomical Journal)
    Full Text Available 
  5. ; ; ; ; ; ; ; ; ; ; et al ( , The Astronomical Journal)
    Full Text Available 
  6. ; ; ; ; ; ; ; ; ; ; et al ( , The Astronomical Journal)
    Full Text Available 
  7. ; ; ; ; ; ; ; ; ; ; et al ( , Nature)
    Full Text Available 
  8. ; ; ; ; ; ; ; ; ; ; et al ( , The Astronomical Journal)
    Full Text Available 
  9. ; ; ; ; ; ; ; ; ; ; et al ( , The Astronomical Journal)
    Abstract We present the occurrence rates for rocky planets in the habitable zones (HZs) of main-sequence dwarf stars based on the Kepler DR25 planet candidate catalog and Gaia-based stellar properties. We provide the first analysis in terms of star-dependent instellation flux, which allows us to track HZ planets. We define η ⊕ as the HZ occurrence of planets with radii between 0.5 and 1.5 R ⊕ orbiting stars with effective temperatures between 4800 and 6300 K. We find that η ⊕ for the conservative HZ is between (errors reflect 68% credible intervals) and planets per star, while the optimistic HZmore »occurrence is between and planets per star. These bounds reflect two extreme assumptions about the extrapolation of completeness beyond orbital periods where DR25 completeness data are available. The large uncertainties are due to the small number of detected small HZ planets. We find similar occurrence rates between using Poisson likelihood Bayesian analysis and using Approximate Bayesian Computation. Our results are corrected for catalog completeness and reliability. Both completeness and the planet occurrence rate are dependent on stellar effective temperature. We also present occurrence rates for various stellar populations and planet size ranges. We estimate with 95% confidence that, on average, the nearest HZ planet around G and K dwarfs is ∼6 pc away and there are ∼4 HZ rocky planets around G and K dwarfs within 10 pc of the Sun.« less
    Full Text Available 
  10. ; ; ; ; ; ; ; ; ; ; et al ( , The Astronomical Journal)
    Full Text Available