Absolute masses and radii determination in multiplanetary systems without stellar models Article Swipe
J. M. Almenara
,
R. F. Díaz
,
Rosemary A. Mardling
,
S. C. C. Barros
,
C. Damiani
,
G. Bruno
,
X. Bonfıls
,
M. Deleuil
·
YOU?
·
· 2015
· Open Access
·
· DOI: https://doi.org/10.1093/mnras/stv1735
YOU?
·
· 2015
· Open Access
·
· DOI: https://doi.org/10.1093/mnras/stv1735
The masses and radii of extrasolar planets are key observables for\nunderstanding their interior, formation and evolution. While transit photometry\nand Doppler spectroscopy are used to measure the radii and masses respectively\nof planets relative to those of their host star, estimates for the true values\nof these quantities rely on theoretical models of the host star which are known\nto suffer from systematic differences with observations. When a system is\ncomposed of more than two bodies, extra information is contained in the transit\nphotometry and radial velocity data. Velocity information (finite\nspeed-of-light, Doppler) is needed to break the Newtonian $MR^{-3}$ degeneracy.\nWe performed a photodynamical modelling of the two-planet transiting system\nKepler-117 using all photometric and spectroscopic data available. We\ndemonstrate how absolute masses and radii of single-star planetary systems can\nbe obtained without resorting to stellar models. Limited by the precision of\navailable radial velocities (38 $ms^{-1}$), we achieve accuracies of 20 per\ncent in the radii and 70 per cent in the masses, while simulated 1 $ms^{-1}$\nprecision radial velocities lower these to 1 per cent for the radii and 2 per\ncent for the masses. Since transiting multi-planet systems are common, this\ntechnique can be used to measure precisely the mass and radius of a large\nsample of stars and planets. We anticipate these measurements will become\ncommon when the TESS and PLATO mission provide high-precision light curves of a\nlarge sample of bright stars. These determinations will improve our knowledge\nabout stars and planets, and provide strong constraints on theoretical models.\n
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- Type
- article
- Language
- en
- Landing Page
- https://doi.org/10.1093/mnras/stv1735
- https://academic.oup.com/mnras/article-pdf/453/3/2644/13769615/stv1735.pdf
- OA Status
- bronze
- Cited By
- 55
- References
- 42
- Related Works
- 10
- OpenAlex ID
- https://openalex.org/W2287929126
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Raw OpenAlex JSON
- OpenAlex ID
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https://openalex.org/W2287929126Canonical identifier for this work in OpenAlex
- DOI
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https://doi.org/10.1093/mnras/stv1735Digital Object Identifier
- Title
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Absolute masses and radii determination in multiplanetary systems without stellar modelsWork title
- Type
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articleOpenAlex work type
- Language
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enPrimary language
- Publication year
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2015Year of publication
- Publication date
-
2015-09-02Full publication date if available
- Authors
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J. M. Almenara, R. F. Díaz, Rosemary A. Mardling, S. C. C. Barros, C. Damiani, G. Bruno, X. Bonfıls, M. DeleuilList of authors in order
- Landing page
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https://doi.org/10.1093/mnras/stv1735Publisher landing page
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https://academic.oup.com/mnras/article-pdf/453/3/2644/13769615/stv1735.pdfDirect link to full text PDF
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YesWhether a free full text is available
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bronzeOpen access status per OpenAlex
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https://academic.oup.com/mnras/article-pdf/453/3/2644/13769615/stv1735.pdfDirect OA link when available
- Concepts
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Physics, Planet, Exoplanet, Radial velocity, Photometry (optics), Astrophysics, Planetary system, RADIUS, Transit (satellite), Astronomy, Stars, Public transport, Computer science, Political science, Computer security, LawTop concepts (fields/topics) attached by OpenAlex
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55Total citation count in OpenAlex
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2025: 4, 2023: 1, 2022: 3, 2021: 2, 2020: 2Per-year citation counts (last 5 years)
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42Number of works referenced by this work
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10Other works algorithmically related by OpenAlex
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| abstract_inverted_index.masses, | 151 |
| abstract_inverted_index.masses. | 172 |
| abstract_inverted_index.measure | 24, 184 |
| abstract_inverted_index.mission | 208 |
| abstract_inverted_index.models. | 126 |
| abstract_inverted_index.planets | 6, 30 |
| abstract_inverted_index.provide | 209, 229 |
| abstract_inverted_index.stellar | 125 |
| abstract_inverted_index.systems | 119, 176 |
| abstract_inverted_index.transit | 17 |
| abstract_inverted_index.without | 122 |
| abstract_inverted_index.Doppler) | 85 |
| abstract_inverted_index.Velocity | 82 |
| abstract_inverted_index.a\nlarge | 214 |
| abstract_inverted_index.absolute | 112 |
| abstract_inverted_index.obtained | 121 |
| abstract_inverted_index.planets, | 227 |
| abstract_inverted_index.planets. | 196 |
| abstract_inverted_index.relative | 31 |
| abstract_inverted_index.velocity | 80 |
| abstract_inverted_index.$MR^{-3}$ | 92 |
| abstract_inverted_index.Newtonian | 91 |
| abstract_inverted_index.contained | 74 |
| abstract_inverted_index.estimates | 38 |
| abstract_inverted_index.formation | 13 |
| abstract_inverted_index.interior, | 12 |
| abstract_inverted_index.known\nto | 55 |
| abstract_inverted_index.modelling | 97 |
| abstract_inverted_index.models.\n | 234 |
| abstract_inverted_index.per\ncent | 141, 169 |
| abstract_inverted_index.performed | 94 |
| abstract_inverted_index.planetary | 118 |
| abstract_inverted_index.precisely | 185 |
| abstract_inverted_index.precision | 130 |
| abstract_inverted_index.resorting | 123 |
| abstract_inverted_index.simulated | 153 |
| abstract_inverted_index.accuracies | 138 |
| abstract_inverted_index.anticipate | 198 |
| abstract_inverted_index.available. | 109 |
| abstract_inverted_index.evolution. | 15 |
| abstract_inverted_index.extrasolar | 5 |
| abstract_inverted_index.quantities | 44 |
| abstract_inverted_index.systematic | 58 |
| abstract_inverted_index.transiting | 101, 174 |
| abstract_inverted_index.two-planet | 100 |
| abstract_inverted_index.values\nof | 42 |
| abstract_inverted_index.velocities | 133, 157 |
| abstract_inverted_index.$ms^{-1}$), | 135 |
| abstract_inverted_index.constraints | 231 |
| abstract_inverted_index.differences | 59 |
| abstract_inverted_index.information | 72, 83 |
| abstract_inverted_index.observables | 9 |
| abstract_inverted_index.photometric | 105 |
| abstract_inverted_index.single-star | 117 |
| abstract_inverted_index.theoretical | 47, 233 |
| abstract_inverted_index.is\ncomposed | 65 |
| abstract_inverted_index.measurements | 200 |
| abstract_inverted_index.multi-planet | 175 |
| abstract_inverted_index.spectroscopy | 20 |
| abstract_inverted_index.large\nsample | 192 |
| abstract_inverted_index.observations. | 61 |
| abstract_inverted_index.of\navailable | 131 |
| abstract_inverted_index.spectroscopic | 107 |
| abstract_inverted_index.become\ncommon | 202 |
| abstract_inverted_index.determinations | 220 |
| abstract_inverted_index.high-precision | 210 |
| abstract_inverted_index.photodynamical | 96 |
| abstract_inverted_index.We\ndemonstrate | 110 |
| abstract_inverted_index.degeneracy.\nWe | 93 |
| abstract_inverted_index.photometry\nand | 18 |
| abstract_inverted_index.this\ntechnique | 179 |
| abstract_inverted_index.knowledge\nabout | 224 |
| abstract_inverted_index.respectively\nof | 29 |
| abstract_inverted_index.for\nunderstanding | 10 |
| abstract_inverted_index.system\nKepler-117 | 102 |
| abstract_inverted_index.transit\nphotometry | 77 |
| abstract_inverted_index.$ms^{-1}$\nprecision | 155 |
| abstract_inverted_index.(finite\nspeed-of-light, | 84 |
| cited_by_percentile_year.max | 100 |
| cited_by_percentile_year.min | 89 |
| countries_distinct_count | 3 |
| institutions_distinct_count | 8 |
| citation_normalized_percentile.value | 0.97587449 |
| citation_normalized_percentile.is_in_top_1_percent | False |
| citation_normalized_percentile.is_in_top_10_percent | True |