You would think that seven planets around TRAPPIST-1 would be more than enough, but Alan Boss and colleagues at the Carnegie Institution for Science are asking whether this system might not also contain one or more gas giants. It’s a theoretical question given weight by the desire to learn more about planet formation, for if we can find gas giants here, it would give credence to a model of gas giant formation championed by Boss. The team has now put constraints on the mass of any gas giants that might lurk here, a prelude to further study.
The core accretion model is widely accepted as a way to create planets like our Earth. Here, the gas and dust disk surrounding a young star shows slow accretion as small particles begin to clump together, gradually forming into planetesimals and, via collisions and other interactions, eventually assembling planets, along with a great deal of leftover debris.
Core accretion can be modeled and seems to fit what we see in other infant planetary systems, but gas giants continue to raise questions. For a gas giant to form this way, it would have to accrete as a solid core that gradually gained enough mass to attract its dense envelope of surrounding gas. One problem with this is that in the lengthy time required for core accretion, the gaseous disk is also depleted. Unless they form relatively quickly, which core accretion rules out, how would gas giants manage to produce such dense atmospheres?
The theory that Boss has long championed holds that there is a process called disk instability in which the circumstellar disk begins to take on a formation something like the spiral arms of a galaxy. Increasing in mass and density, the largest clumps formed in this way would coalesce — on relatively short timescales — into gas giants. Here’s how he explains disk instability in his 2009 book The Crowded Universe:
Most of the mass contained in gas giant planets is hydrogen and helium gas, with only a minor fraction coming from the iron and silicate rocks that form the bulk of the terrestrial planets. These rocks can take their time in forming a planet such as Earth, but the gas needed for forming gas giant planets is known to disappear from young stars on time scales of a few million years or less. Hence, if a gas giant planet is going to form at all, it must do so before the planet-forming disk’s gas disappears through a combination of being eaten by the voracious young protostar and being blown back out into space by winds and radiation from the protostar or other nearby young stars.
All of that demands a rapid gas giant formation process. TRAPPIST-1 comes into play because it’s a low mass star, some twelve times lower in mass than the Sun. If it can produce a gas giant or two, the onus would be on the core accretion model to explain how the system could have produced it. Boss believes disk instability offers an answer. This is why his team, which includes Proxima Centauri b discoverer Guillem Anglada-Escudé, has made such a close study of TRAPPIST-1, one that may eventually let us make the call on the presence of gas giants.
Image: All seven TRAPPIST-1 planets could easily fit inside the orbit of Mercury, our own Solar System’s innermost planet. Alan Boss and his colleagues investigated whether it’s possible that the TRAPPIST-1 system could contain gas giant planets on much longer-period orbits than the seven known terrestrial ones. Credit: NASA/JPL-Caltech.
Boss and colleagues studied the star with astrometric methods, which measure the position of a star in the sky with accuracy great enough to see the slight changes in motion caused by its planets. Astrometry is hard to do, but its rewards are potentially great, as it can provide accurate estimates of a planet’s mass, a value that challenges other planet detection methods. Unlike radial velocity techniques, astrometry works best at planets on long orbital periods, which makes it ideal for trying to locate gas giants like Jupiter in outer system orbits.
The researchers used Carnegie’s CAPSCam astrometric camera, attached to the 2.5-meter du Pont telescope at Las Campanas Observatory (Chile) to determine the upper limits for gas giants at TRAPPIST-1. The result: There are no planets larger than 4.6 times Jupiter’s mass orbiting the star with a period of one year, and no planets larger than 1.6 times Jupiter’s mass orbiting the star with 5 year periods. Given how tightly packed the TRAPPIST-1 planets are, these are wide orbits, and as Boss says, “There is a lot of space for further investigation between the longer-period orbits we studied here and the very short orbits of the seven known TRAPPIST-1 planets.”
If gas giants are eventually discovered at TRAPPIST-1, would this vindicate disk instability in the formation of such worlds? The paper doesn’t go deeply into the matter:
Montet et al. (2014) combined Doppler and direct imaging results to estimate that about 6.5% of M dwarfs host one or more gas giants within 20 AU. Gas giants orbiting M dwarfs may represent a challenge to the core accretion formation mechanism for gas giant planet formation (e.g., Koshimoto et al. 2014), but not for the competing disk instability mechanism (e.g., Boss 2006).
There is work suggesting that core accretion is less likely as a gas giant formation model around M-dwarfs because core accretion operates more slowly in M-dwarf systems, which would mean an outer gas giant is hard to explain without disk instability — core accretion doesn’t give the gas giant enough time to form. Alan Boss was kind enough to go into the problem more fully in an email this morning:
The classic problem for making gas giants by core accretion around low mass stars is that orbital periods are much longer at a given distance for such low mass stars. Core accretion needs many orbital periods to elapse before collisions result in enough growth to form the cores, and when the orbital period is long enough, the collisions cannot proceed fast enough to grow the cores before the disk gas is dissipated by accretion onto the protostars or by disk winds or photoevaporation etc.
All of this would make any gas giants found around TRAPPIST-1 a likely result of disk instability. Further work on the star using astrometric methods is ongoing and should eventually be able to give us a definitive answer. The team is working to improve its techniques “…with the goal of reducing sources of systematic errors, such as those caused by differential chromatic refraction, and by distortions of the entire optical system that might change with time.”
The paper is Boss et al., “Astrometric Constraints on the Masses of Long-Period Gas Giant Planets in the TRAPPIST-1 Planetary System,” Astronomical Journal Vol. 154, No. 3 (23 August 2017). Abstract / preprint.
I seem to recall that dynamical studies tend to find that gas giants tend to disrupt the kind of tightly-packed, multi-resonant configurations that we see at TRAPPIST-1. If so, this gives another reason not to expect the presence of gas giants around TRAPPIST-1.
Indeed, this is also why some call such compact systems of medium-sized planets ‘anti-Jovian’ systems.
Doesn’t this sound like it ought to be the other way around: “There are no planets larger than 4.6 times Jupiter’s mass orbiting the star with a period of one year, and no planets larger than 1.6 times Jupiter’s mass orbiting the star with 5 year periods”? I would have thought that a further away planet (i.e. with a 5-year period) would be harder to rule out than a nearer one (with a 1-year period), and so while you might be able to rule out a nearby gas giant all the way down to 1.6 m_J, the further-out possibilities could only be constrained to be no bigger than 4.6 m_J. Could someone explain why it’s this way around?
Yes, I’m wondering about this, too!
Michael T
This is an astrometric study, which is sensitive to the size of the sky-projected orbit (in this case, the reflex orbit of the star around the centre-of-mass). This means that objects on wide orbits are easier to detect than close-in ones, provided the orbital period is not too long relative to the timespan of the observations.
This contrasts with the radial velocity method, which is sensitive to the orbital velocity and therefore to close-in orbits (objects on smaller orbits move faster and thus give a larger radial velocity signal) and the transit method which requires that the orbit is sufficiently-well aligned to pass across the disc of the star, which is less probable the further out the object is orbiting.
Thanks – I did realise that the observation method relied on the periodic changes in the star’s position, but I would have thought that surely, for a given mass of planet, a closer orbit would create a bigger tug on the star and cause the star’s orbit around the pair’s center of mass to be wider, thus easier to detect. (Clearly a position further away makes the *planet’s* orbit bigger, and makes the period of the star’s wobbling greater, but I can’t see how it makes the size of the star’s orbit about the center of mass larger…)
The barycenter distance to both bodies increases as the distance between the bodies increases.
Now it makes sense. I should have got it before. While the gravitational force between the star and the planet is less when the planet is further out, their centre of mass is further out and since it’s this that the star revolves around, the star’s periodic motion is easier to detect. Thanks Ron and Andy.
I wouldn’t say easier. As the orbital radius increases the orbital period increases. Thus the velocity and period of the gravitational acceleration decreases, and rapidly at that. There are tremendous technical challenges to be overcome to isolate and verify the signal.
Oops. I meant to say the velocity decreases and the period increases.
Yes, I have to say thanks to you guys, too, as my thinking waa along the same lines.
Astrometric data from GAIA should give us the answer in just a few years.
I wonder if radial velocity measurements of Trappist-1 have been made? Surely if there are massive gas giants orbiting within a few AU of the star then astronomers would have detected the periodic light shifts.
They would have to be made in the infra-red. Optical RV is IMPOSSIBLE with this star because of its EXTREME “redness” and faintness! Currently IR spectrographs are FAR LESS SENSITIVE than optical ones. ALSO: A planet orbiting TRAPPIST-1 at 1 AU takes ALMOST AS LONG to complete an orbit as Jupiter does. A Jupiter-like planet in a Jupiter-like orbit would take ALMOST A CENTURY to complete an orbit.
That’s a bit of an exaggeration in terms of how long the orbits would take. Orbital period at 1 AU for total mass of 0.0802*m_sun+m_jupiter is about 3.5 years (Jupiter’s orbital period is 11.8 years), whereas the orbital period at 5.2 AU is about 41.6 years.
It wasn’t that long ago that all we saw were gas giants–and we ached for smaller worlds.
I’m liking the fact that has been reversed ;)
Paul Gilster: Could you check this out for me: Steinn Sigurdsson posted this VERY INTREGUING TWEET recently. Dr. Rodrego Luger, University of Washington “Probing the TRAPPIST-1 System with planet-planet occultations”@PSUScience#PSUAstro Seminar. What intregues me is that he used the word “WITH” instead of “for”. Has he found any? Keep in mind that a P-PO is where two planets are transiting at the same time, AND THEN, one planet ECLIPSES the other! If you could find and then post the DATE of the seminar, I would appreciate it. Thanks.
Entirely theoretical at this point, from what I can tell, though if I hear anything more, I’ll pass it along. Have asked Dr. Sigurðsson,