CITATION — REFERENCE ENTRY

Exoplanet Detection Methods — Planets, Stars and Stellar Systems

Revision ad7ff438-355d-4804-a8f2-b8648f9d3b05 · 11/5/2026, 10:48:29 PM UTC
Key
wright2012methods
Authors
Wright, Jason T.; Gaudi, B. Scott
Issued
2013
Type
chapter
Container
Planets, Stars and Stellar Systems
Publisher
Springer
Raw CSL JSON
{
  "DOI": "10.1007/978-94-007-5606-9_10",
  "URL": "https://arxiv.org/abs/1210.2471",
  "note": "arXiv:1210.2471",
  "type": "chapter",
  "title": "Exoplanet Detection Methods",
  "author": [
    {
      "given": "Jason T.",
      "family": "Wright"
    },
    {
      "given": "B. Scott",
      "family": "Gaudi"
    }
  ],
  "issued": {
    "date-parts": [
      [
        2013
      ]
    ]
  },
  "accessed": {
    "date-parts": [
      [
        2026,
        11,
        5
      ]
    ]
  },
  "publisher": "Springer",
  "container-title": "Planets, Stars and Stellar Systems"
}

Claims

  1. Each detection method favors different planets: transit surveys favor large planets on short orbits; radial-velocity surveys favor massive planets; ground-based direct imaging favors young, massive planets on wide orbits; microlensing favors planets of more than about 10 Earth masses just beyond the snow line; astrometry favors massive, long-period planets. The methods are strongly complementary.
    Locator: section: 3.1 Sensitivities of the Methods
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