The DOI matches its Crossref record; 9 of the 9 references it cites were found in a registry or an index.
HOW ROCKY ARE THEY? THE COMPOSITION DISTRIBUTION OF KEPLER’S SUB-NEPTUNE PLANET CANDIDATES WITHIN 0.15 AU
Open accessAbstract
The Kepler Mission has found thousands of planetary candidates with radii between 1 and 4 . These planets have no analogues in our own solar system, providing an unprecedented opportunity to understand the range and distribution of planetary compositions allowed by planet formation and evolution. A precise mass measurement is usually required to constrain the possible composition of an individual super-Earth-sized planet, but these measurements are difficult and expensive to make for the majority of Kepler planet candidates (PCs). Fortunately, adopting a statistical approach helps us to address this question without them. In particular, we apply hierarchical Bayesian modeling to a subsample of Kepler PCs that is complete for days and and draw upon interior structure models that yield radii largely independent of mass by accounting for the thermal evolution of a gaseous envelope around a rocky core. Assuming the envelope is dominated by hydrogen and helium, we present the current-day composition distribution of the sub-Neptune-sized planet population and find that H+He envelopes are most likely to be ∼1% of these planets' total masses with an intrinsic scatter of ±0.5 dex. We address the gaseous/rocky transition and illustrate how our results do not result in a one-to-one relationship between mass and radius for this sub-Neptune population; accordingly, dynamical studies that wish to use Kepler data must adopt a probabilistic approach to accurately represent the range of possible masses at a given radius.
Overview
The claims and statistics of this paper haven’t been checked yet.
Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.
Integrity signals
Registry
Cites
Statistics
Verification
Claims the paper makes
The claims and statistics of this paper haven’t been checked yet.
Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.
Self-check
Percentages, sums and reported differences re-computed from the paper’s own numbers.
The self-check needs the paper’s full text.
Citations
Cites
Kepler planet-detection mission: Introduction and first results
Borucki, W. J., Koch, D., Basri, G., Batalha, N., Brown, T., Caldwell, D., Caldwell, J., Christensen-Dalsgaard, J., Cochran, W. D., DeVore, E., et al. (2010) · Science · doi:10.1126/science.1185402 · Cited by 4,035
Borucki, W. J., Koch, D. G., Basri, G., Batalha, N., Brown, T. M., Bryson, S. T., Caldwell, D., Christensen-Dalsgaard, J., Cochran, W. D., DeVore, E., et al. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/736/1/19 · Cited by 1,042
A super-Earth transiting a nearby low-mass star
Charbonneau, D., Berta, Z. K., Irwin, J., Burke, C. J., Nutzman, P., Buchhave, L. A., Lovis, C., Bonfils, X., Latham, D. W., Udry, S., et al. (2009) · Nature · doi:10.1038/nature08679 · Cited by 797
UNDERSTANDING THE MASS-RADIUS RELATION FOR SUB-NEPTUNES: RADIUS AS A PROXY FOR COMPOSITION
Lopez, E. D., & Fortney, J. J. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/792/1/1 · Cited by 722
Self-citationTHE MASS-RADIUS RELATION FOR 65 EXOPLANETS SMALLER THAN 4 EARTH RADII
Weiss, L. M., & Marcy, G. W. (2014) · The Astrophysical Journal · doi:10.1088/2041-8205/783/1/l6 · Cited by 665
The Occurrence and Mass Distribution of Close-in Super-Earths, Neptunes, and Jupiters
Howard, A. W., Marcy, G. W., Johnson, J. A., Fischer, D. A., Wright, J. T., Isaacson, H., Valenti, J. A., Anderson, J., Lin, D. N. C., & Ida, S. (2010) · Science · doi:10.1126/science.1194854 · Cited by 635
THE FREQUENCY OF HOT JUPITERS ORBITING NEARBY SOLAR-TYPE STARS
Wright, J. T., Marcy, G. W., Howard, A. W., Johnson, J. A., Morton, T. D., & Fischer, D. A. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/753/2/160 · Cited by 371 · cited 1×
“…Dressing & Charbonneau 2013; Morton & Swift 2013; Petigura et al. 2013), the consistency between RV and transit surveys (Wolfgang & Laughlin 2012; Wright et al. 2012; Figueira et al. 2012), the Kepler eccentricity distribution (Moorhead et al. 2011; Kane et al. 2012; Wu & Lithwick 2013), and the…”
BackgroundDENSITY AND ECCENTRICITY OF KEPLER PLANETS
Wu, Y., & Lithwick, Y. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/772/1/74 · Cited by 231
An Earth-sized planet with an Earth-like density
Pepe, F., Cameron, A. C., Latham, D. W., Molinari, E., Udry, S., Bonomo, A. S., Buchhave, L. A., Charbonneau, D., Cosentino, R., Dressing, C. D., et al. (2013) · Nature · doi:10.1038/nature12768 · Cited by 220 · cited 3×
“…irradiated planets should have lost their envelopes, which we expect given the well-constrained rocky compositions of Corot-7b (Jackson et al. 2010; Valencia et al. 2010), Kepler-10b (Batalha et al. 2011; Kurokawa & Kaltenegger 2013), and Kepler-78b (Pepe et al. 2013; Howard et al. 2013).”
Background
Cited by
Weiss, L. M., Marcy, G. W., Petigura, E. A., Fulton, B. J., Howard, A. W., Winn, J. N., Isaacson, H. T., Morton, T. D., Hirsch, L. A., Sinukoff, E. J., et al. (2018) · The Astronomical Journal · doi:10.3847/1538-3881/aa9ff6 · Cited by 328
BREEDING SUPER-EARTHS AND BIRTHING SUPER-PUFFS IN TRANSITIONAL DISKS
Lee, E. J., & Chiang, E. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/817/2/90 · Cited by 317
Hot super-Earths stripped by their host stars
Lundkvist, M. S., Kjeldsen, H., Albrecht, S., Davies, G. R., Basu, S., Huber, D., Justesen, A. B., Karoff, C., Silva Aguirre, V., Van Eylen, V., et al. (2016) · Nature Communications · doi:10.1038/ncomms11201 · Cited by 258
The degree of fine-tuning in our universe — and others
Adams, F. C. (2019) · Physics Reports · doi:10.1016/j.physrep.2019.02.001 · Cited by 62
Evidence for Two Hot-Jupiter Formation Paths
Nelson, B. E., Ford, E. B., & Rasio, F. A. (2017) · The Astronomical Journal · doi:10.3847/1538-3881/aa82b3 · Cited by 36
Metadata
- Authors
- Wolfgang, A., & Lopez, E.
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2015-06-17
- Volume
- 806
- Issue
- 2
- Pages
- 183
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W1781644248
- Cited by
- 197
- References
- 9
- FWCI
- 21.22
- Type
- journal article
- Language
- en
- Open access
- bronze
About these checks
Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.
Statistics and arithmetic are recomputed, not judged.
Confidence bands are shown only for fields calibrated on our annotated test set. None is calibrated yet, so no band is shown.
What counts as a claim ›How we measure confidence ›How we check this ›
Are you an author, or do you see a problem with this page? Request a review
How to cite
Cite CoChat for the checks on this page, and the paper for its own findings.
- This page
- CoChat. (2026). Citation check: HOW ROCKY ARE THEY? THE COMPOSITION DISTRIBUTION OF KEPLER’S SUB-NEPTUNE PLANET CANDIDATES WITHIN 0.15 AU. https://app.cochat.ai/papers/10.1088/0004-637x/806/2/183
- The paper
- Wolfgang, A., & Lopez, E. (2015). HOW ROCKY ARE THEY? THE COMPOSITION DISTRIBUTION OF KEPLER’S SUB-NEPTUNE PLANET CANDIDATES WITHIN 0.15 AU. The Astrophysical Journal. https://doi.org/10.1088/0004-637x/806/2/183
Data sources
Bibliographic data: Semantic Scholar, OpenAlex, Crossref.
Contains information from the Semantic Scholar Academic Graph Datasets, made available under the ODC Attribution License (ODC-BY 1.0).
Semantic Scholar’s data is described in: Kinney, R., et al. (2023). The Semantic Scholar Open Data Platform. arXiv:2301.10140.
