HIP 113103 b
HIP 113103 b
confirmed planet • updated: 2023-09-19
HIP 113103 b orbits a star slightly smaller and cooler than our Sun. It was discovered in 2023 by NASA’s TESS satellite, which looks for tiny dips in starlight when planets cross in front of their stars.
This page summarizes a catalog entry. If a measurement is missing, it is not shown or guessed. Some values can differ slightly between studies; when that happens, we describe the range rather than picking a favorite without evidence.
Scientific context
Scientific context: This profile layers interpretation on top of archival measurements. Modeled bands appear where direct detections (like spectra or transits) are not listed.
What we can’t claim: surface conditions, biology, or breathable atmosphere without direct spectra.
This planet orbits its star every 7.6 days, much closer than Earth orbits the Sun. It’s about 1.8 times wider than Earth and likely has a hot surface temperature around 721 Kelvin (about 840°F). Its orbit is slightly oval-shaped, not perfectly circular. We don’t know how heavy it is because the transit method doesn’t measure mass directly.
Glossary (plain English)
- AU: the average Earth–Sun distance.
- Semi-major axis: the planet’s average distance from its star.
- Eccentricity: how oval the orbit is (0 = circle).
- Radial velocity: finding a planet by measuring a star’s tiny “wobble.”
- m·sin i: a minimum mass estimate; the true mass can be higher if the orbit is tilted.
- Equilibrium temperature: a rough estimate from starlight alone, not a surface reading.
HIP 113103 b was first reported in 2023 using the Transit method. The discovery is linked to observations from Transiting Exoplanet Survey Satellite (TESS).
In transit work, astronomers watch for tiny, repeating dips in a star’s light as the planet passes in front of it. Follow-up observations help rule out false positives and refine the orbit.
The catalog lists an orbital period of about 7.61 days, a semi-major axis near 0.069 AU.
The orbit’s eccentricity is 0.17, which describes how stretched the orbit is. Because this is a multi‑planet system, stability is ultimately tested with dynamical (N‑body) fits; catalogs can update as models improve.
A measured mass is not available in this row, which limits what we can infer about composition.
A catalog radius is also listed, which (together with mass) helps constrain density and interior structure.
Why “m·sin i” shows up on RV planets
HIP 113103 b orbits HIP 113103.
A temperature near 4930 K places it on the sun-like side of the main sequence. The system is about 150.7 light‑years away.
Several key parameters are not present in this single catalog row. Missing fields don’t mean the science is unknown—only that this particular snapshot doesn’t carry the values.
In this case the most noticeable gaps are: mass. As new observations arrive, archives often refresh these entries (and sometimes revise earlier numbers).
Scientists keep revisiting systems like this because each new instrument pass can tighten uncertainties: better timing improves the orbit, better spectra improves the star, and better follow‑up can confirm or refute competing solutions. Even when a planet is well‑established, refined stellar properties can shift the inferred planet size, temperature, and habitability context. Transit systems are especially valuable because they can be re‑observed for decades to detect subtle changes in timing or additional planets.