Matching theory to observation often requires creative detective work. In a new study, scientists have used a clever test to reveal clues about the birth of speedy, Earth-sized planets.
Artist’s impression of COROT-7b, an ultra-short-period planet.
Former Hot Jupiters?
Artist’s impression of a hot Jupiter with an evaporating atmosphere.
Among the many different types of exoplanets we’ve observed, one unusual category is that of ultra-short-period planets. These roughly Earth-sized planets speed around their host stars at incredible rates, with periods of less than a day.
How do planets in this odd category form? One popular theory is that they were previously hot Jupiters, especially massive gas giants orbiting very close to their host stars. The close orbit caused the planets’ atmospheres to be stripped away, leaving behind only their dense cores.
In a new study, a team of astronomers led by Joshua Winn (Princeton University) has found a clever way to test this theory.
Planetary radius vs. orbital period for the authors’ three statistical samples (colored markers) and the broader sample of stars in the California Kepler Survey.
Winn et al. 2017
Stars hosting hot Jupiters have an interesting quirk: they typically have metallicities that are significantly higher than an average planet-hosting star. It is speculated that this is because planets are born from the same materials as their host stars, and hot Jupiters require the presence of more metals to be able to form.
Regardless of the cause of this trend, if ultra-short-period planets are in fact the solid cores of former hot Jupiters, then the two categories of planets should have hosts with the same metallicity distributions. The ultra-short-period-planet hosts should therefore also be weighted to higher metallicities than average planet-hosting stars.
To test this, the authors make spectroscopic measurements and gather data for a sample of stellar hosts split into three categories:
- 64 ultra-short-period planets (orbital period shorter than a day)
- 23 hot Jupiters (larger than 4 times Earth’s radius and orbital period shorter than 10 days)
- 243 small hot planets (smaller than 4 times Earth’s radius and orbital period between 1 and 10 days)
They then compare the metallicity distributions of these three groups.
Back to the Drawing Board
Metallicity distributions of the three statistical samples. The hot-Jupiter hosts (orange) have different distribution than the others; it is weighted more toward higher metallicities.
Winn et al. 2017
Winn and collaborators find that hosts of ultra-short-period planets do not have the same metallicity distribution as hot-Jupiter hosts; the metallicities of hot-Jupiter hosts are significantly higher. The metallicity distributions for hosts of ultra-short-period planets and hosts of small hot planets were statistically indistinguishable, however.
These results strongly suggest that the majority of ultra-short-period planets are not the cores of former hot Jupiters. Alternative options include the possibility that they are the cores of smaller planets, such as sub-Neptunes, or that they are the short-period extension of the distribution of close-in, small rocky planets that formed by core accretion.
This narrowing of the options for the formation of ultra-short-period planets is certainly intriguing. We can hope to further explore possibilities in the future after the Transiting Exoplanet Survey Satellites (TESS) comes online next year; TESS is expected to discover many more ultra-short-period planets that are too faint for Kepler to detect.
Joshua N. Winn et al 2017 AJ 154 60. doi:10.3847/1538-3881/aa7b7c
Related Journal Articles
- K2-66b and k2-106b: two extremely hot sub-neptune-size planets with high densities doi: 10.3847/1538-3881/aa725f
- A study of the shortest-period planets found with kepler doi: 10.1088/0004-637X/787/1/47
- Transits and occultations of an earth-sized planet in an 8.5 hr orbit doi: 10.1088/0004-637X/774/1/54
- Planet occurrence within 0.25 au of solar-type stars from kepler doi: 10.1088/0067-0049/201/2/15
- A new model of roche lobe overflow for short-period gaseous planets and binary stars doi: 10.3847/1538-4357/835/2/145
- Masses, radii, and orbits of small kepler planets: the transition from gaseous to rocky planets doi: 10.1088/0067-0049/210/2/20
This article originally appeared on the AAS Nova website.