HR 5183 b
HR 5183 b
confirmed planet • updated: 2019-09-23
HR 5183 b orbits the star HR 5183, which is slightly bigger and hotter than our Sun. Scientists spotted it in 2019 using the radial velocity method, which tracks how the star moves back and forth due to the planet’s gravity.
This page summarizes what’s in the catalog. If a number is missing, it’s not shown — we don’t guess. Some values vary between studies; when that happens, we show the range so you know how much uncertainty exists.
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 has a minimum mass about 3 times that of Jupiter and takes roughly 27,000 days (about 74 Earth years) to complete one orbit. Its path is very oval-shaped (eccentric), meaning it swings far from and then close to its star. Because we only measure the minimum mass (written as m sin i), the real mass could be higher if the orbit is tilted.
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.
HR 5183 b was first reported in 2019 using the Radial Velocity method. The discovery is linked to observations from Multiple Observatories.
Radial-velocity detections come from subtle shifts in the star’s spectrum as it wobbles under the planet’s gravity. The first mass value is often a minimum (m·sin i) unless the orbit’s tilt is known.
The catalog lists an orbital period of about 27000.00 days, a semi-major axis near 18.000 AU.
The orbit’s eccentricity is 0.84, which describes how stretched the orbit is. A higher eccentricity can imply stronger past interactions or migration, and it can matter for long‑term stability in multi‑planet systems.
The archive reports a mass scale of 3.2 MJ.
For radial‑velocity work this is commonly m·sin i (a minimum mass) because the orbital tilt is unknown. A rough radius estimate is shown for UI completeness, but it should not be treated as a measurement.
Why “m·sin i” shows up on RV planets
HR 5183 b orbits HR 5183.
A temperature near 5794 K places it on the sun-like side of the main sequence. The system is about 102.6 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: radius. 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.