HD 284149 AB b
HD 284149 AB b
confirmed planet • updated: 2024-06-11
HD 284149 AB b orbits the star HD 284149 A. It was found using direct imaging — taking actual pictures of the object near the star — from the Paranal Observatory in 2017.
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 26 times that of Jupiter, placing it near the boundary between giant planets and brown dwarfs. It orbits at about 431 times Earth’s distance from the Sun. Because it was found by imaging, we don’t yet know how long its orbit takes or how elliptical it is. Its estimated temperature is around 2395 Kelvin, but this could vary slightly based on different studies.
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.
HD 284149 AB b was first reported in 2017 using the Imaging method. The discovery is linked to observations from Paranal Observatory.
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 a semi-major axis near 431.160 AU.
Eccentricity is not provided here; many catalogs omit it when the solution is underconstrained.
The archive reports a mass scale of 26.3 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
HD 284149 AB b orbits HD 284149 A.
A temperature near 6035 K places it on the hotter side of the main sequence. The system is about 384.2 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, orbital period, eccentricity. 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.