Chapter 2 of 15 · SetuHQ does this
Transit
When a planet crosses its star, it blocks a little light. The dip's depth gives the planet's size relative to the star; its repetition gives the period. This is what SetuHQ does: its run found pi Men c's transits in TESS sector 1. Open SetuHQ's Transit case ›
What shapes the dip
The depth is roughly (Rp/R★)². The star is brighter at its centre than its edge (limb darkening), so the bottom of the dip is rounded, not flat, and a central crossing dips deeper than k² (Mandel & Agol 2002; Claret 2017 coefficients for TESS). The four contact points set the total duration T14 and the flat-bottom duration T23 (Winn 2010).
| Quantity | Value | From |
|---|---|---|
| Rp/R★ (k) | 0.0156 | exoplanet.eu Rp = 0.16719 RJ, R★ = 1.1 R☉ [calc] |
| k² (depth with no limb darkening) | 244 ppm | [calc] |
| Model depth at the stored b | 267 ppm | quadratic limb darkening u₁ = 0.333, u₂ = 0.228 (Claret 2017, 6037 K) [calc] |
| Model depth for a central crossing | 287 ppm | [calc] |
| SetuHQ's fitted depth, lead dip | 294 ppm | setuhq run, limb-darkened fit, mid-transit depth (real data) |
| T14 / T23 | 3.07 h / 2.93 h | Winn 2010 eqs. 14–15 from a/R★ = 13.10, b = 0.5738 [calc]; Huang 2018 publish 2.953 ± 0.047 h |
| Star | G · ≈G0V · rgb(255, 244, 242) | nearest row of Mamajek's sequence; blackbody colour from the CIE 1931 fit |
The curve is a model drawn from stored values (small-planet approximation of Mandel & Agol 2002, circular orbit), not observed data. The dots are SetuHQ's own stored points for its lead dip. The orbit is not to scale; its tilt is set so the planet crosses at the stored impact parameter.
4,790 of the 8,049 planets with a stored distance in exoplanet.eu were found by transit (the first method listed). Show them on the Galaxy map ›
peak 1,450 (2016)
19882026
Sources
- Winn 2010, Transits and occultations
- Mandel & Agol 2002, ApJ 580, L171
- Claret 2017, A&A 600, A30 (TESS limb darkening)
- Huang et al. 2018, ApJL 868, L39 (pi Men c)
- Pecaut & Mamajek 2013, ApJS 208, 9 (dwarf sequence, v2022.04.16)
- Wyman, Sloan & Shirley 2013, JCGT 2(2) (CIE fit)
- Prša et al. 2016, AJ 152, 41 (IAU 2015 B3 nominal values)