HIP 39017 b
HIP 39017 b
confirmed planet • updated: 2024-04-19
HIP 39017 b was spotted directly by telescopes in 2024, orbiting the star HIP 39017. This method lets us see the object itself, not just its effect on the star.
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 object has a mass about 23.6 times that of Jupiter and orbits its star at a distance of roughly 22 astronomical units. Its orbit is very stretched out (eccentricity of 0.55), meaning it swings far from and close to its star over its 31,000-day orbit. Because it was imaged directly, we know its mass is real—not a minimum estimate—but its size and surface temperature are not available.
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 39017 b was first reported in 2024 using the Imaging method. The discovery is linked to observations from Multiple Observatories.
Direct imaging tries to separate faint planetary light from the glare of the host star. It works best for young, warm planets far from their stars.
The catalog lists an orbital period of about 31000.00 days, a semi-major axis near 22.100 AU.
The orbit’s eccentricity is 0.55, 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 23.6 MJ.
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
HIP 39017 b orbits HIP 39017.
The star is classified as A9/F0, which is a shorthand for temperature and color. The system is about 216.3 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, catalog equilibrium temperature. 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.