HD 97048 b
HD 97048 b
derived planet • updated: 2019-10-18
HD 97048 b orbits the young star HD 97048. Scientists detected it using the disk kinematics method with the ALMA telescope, which looks for disturbances in the planet-forming disk around 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.
The catalog lists a planet with a mass about 2.5 times that of Jupiter, orbiting at about 130 times Earth’s distance from the Sun. Because it was found using disk kinematics, we don’t yet know its exact orbit length or shape. The star is hot and bright, about 2.4 times the mass of our Sun.
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 97048 b was first reported in 2019 using the Disk Kinematics method.
The discovery is linked to observations from Atacama Large Millimeter Array (ALMA). Different methods emphasize different strengths: some constrain size, some constrain mass, and some constrain both.
The catalog lists a semi-major axis near 130.000 AU.
Eccentricity is not provided here; many catalogs omit it when the solution is underconstrained.
The archive reports a mass scale of 2.5 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 97048 b orbits HD 97048. The star is classified as Be9.5/AO, which is a shorthand for temperature and color.
A temperature near 10000 K places it on the hotter side of the main sequence. The system is about 599.7 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: radius, catalog equilibrium temperature, 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.