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Exoplanet Stuff

Fomalhaut b:
Exoplanet Apparently Disappears in Latest Hubble Observations
A team of researchers from the University of Arizona believe a full-grown planet never existed in the first place. Instead, they concluded that the Hubble Space Telescope was looking at an expanding cloud of very fine dust particles from two icy bodies that smashed into each other. Hubble came along too late to witness the suspected collision, but may have captured its aftermath. This happened in 2008, when astronomers eagerly announced that Hubble took its first image of a planet orbiting another star. The diminutive-looking object appeared as a dot next to a vast ring of icy debris encircling Fomalhaut. In following years, they tracked the planet along its trajectory. But over time the dot, based on their analysis of Hubble data, got fainter until it simply dropped out of sight, say the researchers, as they pored through the Hubble archival data.

Earth-Size, Habitable Zone Planet Found Hidden in Early NASA Kepler Data – Exoplanet Exploration: Planets Beyond our Solar System - another one on that planet.

ESA - Cheops observes its first exoplanets and is ready for science
Cheops, ESA’s new exoplanet mission, has successfully completed its almost three months of in-orbit commissioning, exceeding expectations for its performance. The satellite, which will commence routine science operations by the end of April, has already obtained promising observations of known exoplanet-hosting stars, with many exciting discoveries to come.

...
Launched in December 2019, Cheops, or the Characterising Exoplanet Satellite, opened its eye to the Universe at the end of January and shortly after took its first, intentionally blurred images of stars. The deliberate defocusing is at the core of the mission’s observing strategy, which improves the measurement precision by spreading the light coming from distant stars over many pixels of its detector.
 
Impossible Moons - YouTube - only one exomoon candidate. One can search for them using Transit Timing Variations and Transit Duration Variations, and Prof David Kipping narrows down possible exomoon planets by looking for TTV's and TDV's that indicate too-slow periods, more than some fraction of their planet's period.

I will estimate what fraction from the Solar System's moons.
[TABLE="class: grid"]
[TR]
[TD]Planet[/TD]
[TD]Direct[/TD]
[TD]PP/PM[/TD]
[TD]Retrograde[/TD]
[TD]PP/PM[/TD]
[/TR]
[TR]
[TD]Earth[/TD]
[TD]Moon[/TD]
[TD]13.37
[/TD]
[TD][/TD]
[TD][/TD]
[/TR]
[TR]
[TD]Mars[/TD]
[TD]Deimos[/TD]
[TD]543.9
[/TD]
[TD][/TD]
[TD][/TD]
[/TR]
[TR]
[TD]Jupiter
[/TD]
[TD]Valetudo
[/TD]
[TD]8.14
[/TD]
[TD]S/2017 J 1
[/TD]
[TD]5.55
[/TD]
[/TR]
[TR]
[TD]Saturn[/TD]
[TD]S/2004 S 24
[/TD]
[TD]8.31
[/TD]
[TD]S/2004 S 26
[/TD]
[TD]6.61
[/TD]
[/TR]
[TR]
[TD]Uranus[/TD]
[TD]Margaret
[/TD]
[TD]18.55
[/TD]
[TD]Ferdinand
[/TD]
[TD]10.98
[/TD]
[/TR]
[TR]
[TD]Neptune[/TD]
[TD]Laomedeia
[/TD]
[TD]18.92
[/TD]
[TD]Neso
[/TD]
[TD]6.33
[/TD]
[/TR]
[TR]
[TD]Pluto[/TD]
[TD]Hydra
[/TD]
[TD]2371.
[/TD]
[TD][/TD]
[TD][/TD]
[/TR]
[/TABLE]
For direct / prograde moons (orbiting same direction as the planet), the minimum P(planet)/P(moon) is about 8, while for retrograde ones (orbiting in the opposite direction from the planet), the minimum is about 5.5. The  Hill sphere limit is sqrt(3) ~ 1.73.
 
An upper limit to a moon's period is its planet's "surface satellite" period. For the Earth, that is about 1.406 hours. It scales as 1/sqrt(average-density)

But a moon close to its planet could get pulled apart, and with not much internal rigidity, the closest that a moon can get is the  Roche limit. It is a distance of

2.455 * (radius) * sqrt(density-of-planet/density-of-moon)

That gives a period of

3.847 * (surface-satellite period for the moon)

Working out the numbers for habitable-zone planets orbiting red dwarfs, one finds that they are unlikely to have moons.
 
The Weirdest Solar System We've Found So Far? You May Be In It – Exoplanet Exploration: Planets Beyond our Solar System
Before we found the first exoplanets — planets orbiting other stars — it seemed reasonable to suppose that other planetary systems looked like ours: small, rocky planets close to a Sun-like star, a big Jupiter and a few other gas giants farther out.

But after a quarter century of discovery revealing thousands of exoplanets in our galaxy, things look very different. In a word, we are “weird” — at least among the planetary systems found so far.
Part of the problem is what are the easiest kinds of planets to detect. The Solar System's planets turn out to be on the margins of detectability with present-day technology. Jupiter is the easiest to detect by both radial velocity and transits, but its transit probability is a little less than 1/1000, and its period is nearly 12 (Earth) years. So if one wants 3 full orbits, one needs nearly 40 years of observing.

The closest thing to the orbital resonances that many exoplanets have is the "Great Inequality" of Jupiter and Saturn, with their 2:5 orbital resonance. It has a period of about 900 years and an amplitude of about a degree.

How Amateurs Could Help Future Exoplanet Observations - Sky & Telescope - Sky & Telescope

Space observatories like the upcoming James Webb Space Telescope may need to be scheduled down to the minute, and for doing that, one needs very accurate orbits of exoplanets.
Getting that timing right for any given planet will depend on accurate predictions of future transits. But those predictions are only as good as the uncertainties inherent in existing observations. And that’s where amateur astronomers can help, says Robert Zellem (JPL). In a paper posted March 23rd to arXiv.org, he and colleagues propose that citizen scientists with small telescopes can keep transit observations “fresh,” thus reducing wasted time on James Webb and similar missions.

“I know there’s a ton of amateur astronomers out there that have really nice telescopes and that are capable of doing really high-precision observations,” says Zellem. “Even with a small 6-inch telescope, you can get really nice light curves.”
 
space movies | Medium

"This list was made by The Exoplanets Channel, a youtube channel about habitable exoplanets, extraterrestrial intelligence and interstellar travel. ... The list does not follow any specific order."

22. Approaching the unknown
21. Stranded
20. Armageddon
19. The Arrival
18. Apollo 18
17. Life
16. The Last Days on Mars
15. First Man
14. Solaris
13. Europa Report
12. Event Horizon
11. Red Planet
10. Sunshine
9. Ad Astra
8. Moon
7. Mission to Mars
6. Arrival
5. Gravity
4. The Martian
3. Contact
2. Passengers
1. Interstellar

BONUS:
2001: A Space Odyssey
The Right Stuff
Apollo 13
Space Cowboys
Alien
 
Peering Into the Atmosphere of the Hottest Planet Known - KELT-9b
KELT-9b is an extreme world. Clocking in with a dayside temperature of more than 4,500 K (~7,600 °F), it is the hottest planet known — hotter than many stars! This ultra-hot Jupiter orbits at a mere 0.035 AU from its scalding A- or B-type host star, whizzing around its host in just 1.5 days.

The intense radiation bombarding KELT-9b almost certainly takes a toll: this energetic light should dissociate molecules into their component atoms and ionize metals in the hot atmosphere, and it may inflate the envelope of hydrogen gas around the planet to the point where the hot gas escapes.
Detection of Ionized Calcium in the Atmosphere of the Ultra-hot Jupiter KELT-9b - IOPscience

You’ve Got a Friend in Me: A Hot Jupiter with a Unique Companion | astrobites
noting
[2003.10852] TESS spots a hot Jupiter with an inner transiting Neptune
The host star, TOI-1130, is an 11th magnitude K-dwarf in the Gaia G band. It has two transiting planets: a Neptune-sized planet (3.65±0.10 RE) with a 4.1-day period, and a hot Jupiter (1.50+0.27−0.22 RJ) with an 8.4-day period. Precise radial-velocity observations show that the mass of the hot Jupiter is 0.974+0.043−0.044 MJ. For the inner Neptune, the data provide only an upper limit on the mass of 0.17 MJ (3σ).
This could give us some clues on how "hot Jupiters" formed. The first article stated that it was counterevidence for the migration theory, but I note the resonance between the two planets. That suggests that the Jupiter-sized planet could have pushed in the Neptune-sized one.

WFIRST Will Use Warped Space-time to Help Find Exoplanets – Exoplanet Exploration: Planets Beyond our Solar System - with gravitational microlensing. That requires looking at a LOT of stars in the hope that some planet may pass near its line of sight and distort its light. But to date, 96 planets have been discovered by this means.
 
Come on Feel the Noise (Floor) feat. PLATO | astrobites
noting
[2002.08072v1] The Stellar Variability Noise Floor for Transiting Exoplanet Photometry with PLATO

Uses a simulated transit of the Sun by the Earth and estimates how much variability it will have from the Sun's surface granules and its starquakes.  Granule (solar physics) - "A typical granule has a diameter on the order of 1,500 kilometres (930 mi)[1] and lasts 8 to 20 minutes before dissipating.[2] At any one time, the Sun's surface is covered by about 4 million granules. Below the photosphere is a layer of "supergranules" up to 30,000 kilometres (19,000 mi) in diameter with lifespans of up to 24 hours."

The variation induced by this mechanism is about 3.6%, comparable to the expected precision of proposed exoplanet observation satellite PLATO: 3%.

Two Planets Straddling the Gap - the "Fulton gap" of about 1.5 to 2 Earth radii.
noting
The Transiting Multi-planet System HD15337: Two Nearly Equal-mass Planets Straddling the Radius Gap - IOPscience
With an orbital period of 4.8 days, a mass of ${7.51}_{-1.01}^{+1.09}\,{M}_{\oplus }$ and a radius of 1.64 ± 0.06 R ⊕, HD 15337 b joins the growing group of short-period super-Earths known to have a rocky terrestrial composition. The sub-Neptune HD 15337 c has an orbital period of 17.2 days, a mass of ${8.11}_{-1.69}^{+1.82}\,{{\rm{M}}}_{\oplus }$, and a radius of 2.39 ± 0.12 R ⊕, suggesting that the planet might be surrounded by a thick atmospheric envelope. The two planets have similar masses and lie on opposite sides of the radius gap, and are thus an excellent testbed for planet formation and evolution theories.

Earth’s own evolution used as guide to hunt exoplanets | Cornell Chronicle
noting
High-resolution Transmission Spectra of Earth Through Geological Time - IOPscience
I may have posted on it earlier. "Kaltenegger and her team created atmospheric models that match the Earth of 3.9 billion years ago, a prebiotic Earth, when carbon dioxide densely cloaked the young planet. A second throwback model chemically depicts a planet free of oxygen, an anoxic Earth, going back 3.5 billion years. Three other models reveal the rise of oxygen in the atmosphere from a 0.2% concentration to modern-day levels of 21%."
 
Water Transport Throughout The TRAPPIST-1 System: The Role Of Planetesimals - Astrobiology
noting
[2007.05366] Water transport throughout the TRAPPIST-1 system: the role of planetesimals

Outside of the "snow line", a lot of icy planetesimals had likely formed. In the TRAPPIST-1 system, at least, the inner part of the planetesimal belt was likely scattered inward, contributing water to the more inward planets.

The Dynamic Proto-atmospheres Around Low-Mass Planets With Eccentric Orbits - Astrobiology
noting
[2007.04398] The Dynamic Proto-atmospheres around Low-Mass Planets with Eccentric Orbits
"To sum up, low-mass eccentric planets can retain small proto-atmospheres despite the stripping effects of bow shocks. The atmospheres are always connected to and interacting with the disk gas. These findings provide important insights into the impacts of migration and scattering on planetary proto-atmospheres."

KELT-9b: ‘Gravity Darkening’ and an Asymmetric Light Curve
Gravity darkening? KELT-9 rotates with a period of roughly 16 hours, and that star gets a noticeable equatorial bulge. This produces "gravity darkening" at the equator and "gravity brightening" at the poles.

KELT-9b is about 2.9 times Jupiter's mass, its orbit period is 36 hours, and its temperature goes up to 4,600 K on its daytime side (KELT-9's is 9,000 K).
We get a temperature differential of almost 800 degrees Celsius. The effects on the transit light curve are interesting. Beginning near the star’s poles, the transit blocks less light as KELT-9b travels over the stellar equator. We have an asymmetry here we can work with to gain information about the temperature and brightness changes over the surface of the star, learning more about its shape and orientation.

...
A planet like this is going to be useful for research into hot Jupiters. There is a clear trend among such worlds in that they are often spin-orbit misaligned ...

Models of rapidly rotating stars are still being developed, but will be needed to analyze the high number of such stars expected to be discovered by TESS. In fact, I was surprised to learn that in a previous paper, lead author John Ahlers (NASA GSFC) had estimated on the order of 2,000 exoplanets will turn up orbiting A/F stars in the TESS data, and the expectation is that a large number of these will be spin-orbit misaligned. Thus KELT-9b gives us a window into fast rotators, which are expected to comprise a large number of the A/F systems discovered.
noting
KELT-9 b's Asymmetric TESS Transit Caused by Rapid Stellar Rotation and Spin–Orbit Misalignment - IOPscience
We constrain the host star's equatorial radius to be 1.089 ± 0.017 times as large as its polar radius and its local surface brightness to vary by ~38% between its hot poles and cooler equator. We model the stellar oblateness and surface brightness gradient and find that it causes the transit light curve to lack the usual symmetry around the time of minimum light. We take advantage of the light-curve asymmetry to constrain KELT-9 b's true spin–orbit angle (${87^\circ }_{{-11}^{^\circ }}^{{+10}^{^\circ }}$), agreeing with Gaudi et al. that KELT-9 b is in a nearly polar orbit.
 
Orbiting close to a fast-rotating star. That made me think. The star would have a sizable equatorial bulge, and that bulge would cause the planet's orbit to precess. I'm a sucker for celestial-mechanics effects, so I looked for evidence of that in the literature, or at least estimates of that.

MEASUREMENT OF THE NODAL PRECESSION OF WASP-33 b VIA DOPPLER TOMOGRAPHY - IOPscience
Doppler tomographic measurement of the nodal precession of WASP-33b | Publications of the Astronomical Society of Japan | Oxford Academic
Using equations of long-term orbital precession, we constrain the stellar gravitational quadrupole moment J2 = (9.14 ± 0.51) × 10−5 and the angle between the stellar spin axis and the line of sight i⋆=96+10−14 deg. These updated values show that the host star is more spherical and viewed more equator than the previous study. We also estimate that the precession period is ∼840 yr. We also find that the precession amplitude of WASP-33b is ∼67° and WASP-33b transits in front of the host star for only ∼20% of the whole precession period.

MEASUREMENT OF SPIN-ORBIT MISALIGNMENT AND NODAL PRECESSION FOR THE PLANET AROUND PRE-MAIN-SEQUENCE STAR PTFO 8-8695 FROM GRAVITY DARKENING - IOPscience

Spin-Orbit Alignment: A Lesson from Beta Pictoris?
Spin–Orbit Alignment of the β Pictoris Planetary System - IOPscience
[2006.10784] Spin-orbit alignment of the $β$ Pictoris planetary system
"The angular momentum vectors of the stellar photosphere, the planet, and the outer debris disk are well-aligned with mutual inclinations <3±5∘, which indicates that β Pic b formed in a system without significant primordial misalignments."

As one would expect from planets condensing from leftover material orbiting a star after its formation. That's what we find here in the Solar System.
 
Some exoplanets may be covered in weird water between liquid and gas | Science News
Now, new simulations indicate that some planets that look like gaseous mini-Neptunes could actually be rocky planets covered in superheated oceans, where the water is in an exotic state between liquid and gas. Such extreme saunalike worlds could bridge the divide between rocky and gaseous planet types, researchers report in the June 15 Astrophysical Journal Letters.
noting
Irradiated Ocean Planets Bridge Super-Earth and Sub-Neptune Populations - IOPscience

[1805.01478] Can Rocky Exoplanets with Rings Pose as Sub-Neptunes?
I'd posted on this about Jupiter-sized planets, but could this also be true of Earth-sized ones?


Colors of an Earth-like Exoplanet - Temporal Flux And Polarization Signals Of The Earth - Astrobiology
noting
[2007.15624] Colors of an Earth-like exoplanet -- Temporal flux and polarization signals of the Earth
Light becomes polarized when it is scattered or reflected, and this polarization can supply clues on what is scattering or reflecting the light. The authors simulated Earthlike planets and found that the polarization was linear, typical of scattering and reflecting, typically around 10% of total intensity, and with only small changes of direction (~ 1%). "Clouds modify but do not completely suppress the variations that are due to rotating surface features."

Seems like an extension of Simulations of Light Curves from Earth-like Exoplanets - Planetary Habitability Laboratory @ UPR Arecibo - one can see the Sahara Desert over interstellar space - it changes the Earth's overall color from bluish to neutral.
 
UK researchers use breakthrough AI to identify 50 new planets from old NASA data - CNN
They trained the AI on known planets and known false positives, then they used it on putative planets listed as unconfirmed.

Referring to
Exoplanet Validation with Machine Learning: 50 new validated Kepler planets | Monthly Notices of the Royal Astronomical Society | Oxford Academic


Formalde-hyde and Seek - where one finds H2CO in protoplanetary disks.

Noting [2002.12525] An ALMA Survey of H$_2$CO in Protoplanetary Disks


Tuning In to Reveal Stellar Wobbles - detection of a planet with astrometry, observing the star's position over time. One has to sort out the star's "proper motion" (its motion through interstellar space) and the Earth's parallax. This one is only the second planet reliably detected with astrometry.

I'm old enough to remember Peter Van de Kamp's claimed astrometric detection of planets orbiting Barnard's Star. That detection is now discredited, in part because telescope maintenance produced a large observed effect.

Noting [2008.01595] An astrometric planetary companion candidate to the M9 Dwarf TVLM 513-46546 - Saturn-mass, at 0.3 AU, with a period of 221 days. I estimate the planet's equilibrium temperature as 83 K, roughly that of Saturn in our Solar System.

The observations were done with the VLBA radio telescope (Very Long Baseline Array). Combining the signals of telescopes across our planet's size gives the effect of a Earth-sized telescope, and that is what enabled the precision of the astrometric measurements that were used in this planet search.
 
The Impact of Land on an Ocean World’s Habitability - "Ocean heat transport in the authors’ models for varying continent size; from top to bottom, continents (noted as the white rectangle in the figure) cover 0%, 4%, 22%, and 39% of the planet surface. Continents at the substellar point inhibit ocean heat transport. [Adapted from Salazar et al. 2020]"

Noting The Effect of Substellar Continent Size on Ocean Dynamics of Proxima Centauri b - IOPscience - "Our work suggests that both a dynamic ocean and continents are unlikely to decrease the habitability prospects of nearby tidally locked targets like Proxima Centauri b that could be investigated with future observations by the James Webb Space Telescope."


Opportunities from a Newly Discovered Planetary System - two puffy planets (or ringed planets)

Noting The Multiplanet System TOI-421: A Warm Neptune and a Super Puffy Mini-Neptune Transiting a G9 V Star in a Visual Binary - IOPscience


Featured Image: Evidence for Planets in Disks? - protoplanets making gaps in disks. That also happens to planets' rings in the Solar System - Saturn's moons make gaps in the planet's rings.

Noting Nine Localized Deviations from Keplerian Rotation in the DSHARP Circumstellar Disks: Kinematic Evidence for Protoplanets Carving the Gaps - IOPscience
 
Exoplanets at Reddit


Heavy-metal Jupiters | astrobites
noting
[2006.12500] Heavy-metal Jupiters by major mergers: metallicity vs. mass for giant planets

A common scenario of the formation of giant planets is a core that then accreted a lot of volatiles and not much more core material. But several giant planets running into each other can give the resulting planets very big cores.


What’s the largest planet in the Universe? | by Ethan Siegel | Starts With A Bang! | Medium - "You might think Jupiter is large, but you’ll be surprised at what happens if you try and make it larger!"

At around 80 Jupiter masses, it will do H -> He in its core. At around 14 Jupiter masses, it will do deuterium fusion, becoming a brown dwarf.
In terms of physical size, however, brown dwarfs are actually smaller than the largest gas giants.

Above a certain mass, the atoms inside large planets will begin to compress so severely that adding more mass will actually shrink your planet.

This happens in our Solar System, explaining why Jupiter is three times Saturn’s mass, but only 20% physically larger.
An approximate mass-radius relationship:
  • R ~ M^(0.28) -- Terran worlds
  • M = 2 M-E, R = 1.2 R-E - volatile envelope
  • R ~ M^(0.59) -- Neptunian worlds
  • M = 0.41 M-J, R = 12 R-E - self-compression
  • R ~ M^(-0.04) -- Jovian worlds
  • M = 0.08 M-S, R = 11 R-E -- hydrogen burning
  • R ~ M^(0.88) -- stellar worlds
In the absence of hydrogen burning, one gets a white dwarf. For instance, Sirius B has a mass close to the Sun's mass and a radius close to the Earth's radius. Its mass-radius curve is R ~ M^(-1/3) up to a WD's maximum mass, about 1.44 solar masses, the Chandrasekhar mass. There it drops off very fast.

A neutron star is stable with that mass, and a NS's maximum mass is estimated at roughly 2 solar masses.

A black hole has no maximum mass.
 
NASA's TESS Completes Primary Mission | NASA
On July 4, NASA’s Transiting Exoplanet Survey Satellite (TESS) finished its primary mission, imaging about 75% of the starry sky as part of a two-year-long survey. In capturing this giant mosaic, TESS has found 66 new exoplanets, or worlds beyond our solar system, as well as nearly 2,100 candidates astronomers are working to confirm.

...
TESS monitors 24-by-96-degree strips of the sky called sectors for about a month using its four cameras. The mission spent its first year observing 13 sectors comprising the southern sky and then spent another year imaging the northern sky.

Now in its extended mission, TESS has turned around to resume surveying the south. In addition, the TESS team has introduced improvements to the way the satellite collects and processes data. Its cameras now capture a full image every 10 minutes, three times faster than during the primary mission. A new fast mode allows the brightness of thousands of stars to be measured every 20 seconds, along with the previous method of collecting these observations from tens of thousands of stars every two minutes. The faster measurements will allow TESS to better resolve brightness changes caused by stellar oscillations and to capture explosive flares from active stars in greater detail.

These changes will remain in place for the duration of the extended mission, which will be completed in September 2022. After spending a year imaging the southern sky, TESS will take another 15 months to collect additional observations in the north and to survey areas along the ecliptic – the plane of Earth’s orbit around the Sun – that the satellite has not yet imaged.
Good job. With more to come.
 
ESA - First results from Cheops: ESA’s exoplanet observer reveals extreme alien world
noting journal article
The hot dayside and asymmetric transit of WASP-189 b seen by CHEOPS | Astronomy & Astrophysics (A&A)
with
PDF (4.437 MB)

ESA's space telescope CHEOPS is intended to do followup observations of already-known exoplanets. It has recently observed directly a planet called WASP-189b, a superhot Jovian planet detected by its transits of its star. This direct observation is from observing the planet's "secondary transit", going behind the star. The planet is so close that it is hot enough to glow in visible light, and the planet's glow makes a noticeable secondary-transit dip, when it is hidden by its star.

The star WASP-189 is A-type star HD 133112, with apparent visual magnitude 6.6. It has a mass of 2 solar masses and a radius of 2.4 solar radii. Its photosphere temperature is around 8000 K, 2000 K hotter than the Sun's and enough to make it look bluish. It rotates with a period of around 30 hours, enough to give it a noticeable equatorial bulge and to make its poles noticeably hotter than its equator.

The planet has a mass of 2 Jupiter masses and a radius of 1.6 Jupiter radii, and its brightness temperature is 3,400 K. That is hot enough to melt or decompose nearly anything. Only a few chemical elements, like tungsten and carbon, remain solid at that temperature. It gets that hot from orbiting at 4.6 times its star's radius, or 0.05 AU. Its orbit period is 2.72 days and its orbit is very close to circular.

The planet's orbit is nearly polar (inclination 85 d to its star's equator), its orbit is inclined 86 d to the line of sight, and its star's orbit inclined 76 d. With the star going at different brightnesses from its poles to its equator, this produces an asymmetry in the planet's primary-occultation light curve. The planet hides different parts of the star as it travels.


CHEOPS will do many more of this sort of observation of known exoplanets, getting more detail about them.
 
95 Nearby Cool Brown Dwarfs Identified - most of them between 30 and 60 light years away (10 to 20 parsecs).
The data used in the brown dwarf collection come from a range of observatories including W. M. Keck, Mont Mégantic, Las Campanas, Kitt Peak and Cerro Tololo. Space-based data from WISE (Wide-field Infrared Survey Explorer) were also valuable, as were follow-up observations from the Spitzer Space Telescope providing photometric confirmation. Low temperature brown dwarfs like these build our catalog while also clarifying gaps in the low-temperature population.

Jackie Faherty (American Museum of Natural History) is a co-author of the paper, whose lead author is Aaron Meisner (NSF NOIRLab). Faherty places the work in context, while giving a nod to the Backyard Worlds participants:

“This paper is evidence that the solar neighborhood is still uncharted territory and citizen scientists are excellent astronomical cartographers. Mapping the coldest brown dwarfs down to the lowest masses gives us key insights into the low-mass star formation process while providing a target list for detailed studies of the atmospheres of Jupiter analogs.”
The search's home page:
Backyard Worlds: Planet 9 — Zooniverse
 
An ultrahot Neptune in the Neptune desert | Nature Astronomy
About 1 out of 200 Sun-like stars has a planet with an orbital period shorter than one day: an ultrashort-period planet1,2. All of the previously known ultrashort-period planets are either hot Jupiters, with sizes above 10 Earth radii (R⊕), or apparently rocky planets smaller than 2 R⊕. Such lack of planets of intermediate size (the ‘hot Neptune desert’) has been interpreted as the inability of low-mass planets to retain any hydrogen/helium (H/He) envelope in the face of strong stellar irradiation. Here we report the discovery of an ultrashort-period planet with a radius of 4.6 R⊕ and a mass of 29 M⊕, firmly in the hot Neptune desert. Data from the Transiting Exoplanet Survey Satellite3 revealed transits of the bright Sun-like star LTT 9779 every 0.79 days. The planet’s mean density is similar to that of Neptune, and according to thermal evolution models, it has a H/He-rich envelope constituting 9.0+2.7−2.9% of the total mass. With an equilibrium temperature around 2,000 K, it is unclear how this ‘ultrahot Neptune’ managed to retain such an envelope. Follow-up observations of the planet’s atmosphere to better understand its origin and physical nature will be facilitated by the star’s brightness (Vmag = 9.8).
A common hypothesis for this bimodal distribution is that Jovian planets spiral in very close, and then their stars strip off their outer layers, leaving rocky planets. I think that superhot Neptunian planets are planets that were caught late in their outer-layer stripping, when their outer layers are mostly gone but not all gone.

This hypothesis can be tested by finding more of such planets and then checking if their mass and size distributions fit what one would expect from being stripping intermediates.
 
An ultrahot Neptune in the Neptune desert | Nature Astronomy
About 1 out of 200 Sun-like stars has a planet with an orbital period shorter than one day: an ultrashort-period planet1,2. All of the previously known ultrashort-period planets are either hot Jupiters, with sizes above 10 Earth radii (R⊕), or apparently rocky planets smaller than 2 R⊕. Such lack of planets of intermediate size (the ‘hot Neptune desert’) has been interpreted as the inability of low-mass planets to retain any hydrogen/helium (H/He) envelope in the face of strong stellar irradiation. Here we report the discovery of an ultrashort-period planet with a radius of 4.6 R⊕ and a mass of 29 M⊕, firmly in the hot Neptune desert. Data from the Transiting Exoplanet Survey Satellite3 revealed transits of the bright Sun-like star LTT 9779 every 0.79 days. The planet’s mean density is similar to that of Neptune, and according to thermal evolution models, it has a H/He-rich envelope constituting 9.0+2.7−2.9% of the total mass. With an equilibrium temperature around 2,000 K, it is unclear how this ‘ultrahot Neptune’ managed to retain such an envelope. Follow-up observations of the planet’s atmosphere to better understand its origin and physical nature will be facilitated by the star’s brightness (Vmag = 9.8).
A common hypothesis for this bimodal distribution is that Jovian planets spiral in very close, and then their stars strip off their outer layers, leaving rocky planets. I think that superhot Neptunian planets are planets that were caught late in their outer-layer stripping, when their outer layers are mostly gone but not all gone.

This hypothesis can be tested by finding more of such planets and then checking if their mass and size distributions fit what one would expect from being stripping intermediates.
I have this weird feeling we need about 10,000 solar systems before we get a feel for how they work. Even then, we really can't rewind the clock on them.

Originally, it is such a violent process to begin with and then you have interactions from other extra solar objects that can screw things up. How often those extra solar objects do as such might be much more common than we appreciate, once every million or ten million years or something. Heck, we have a rogue star coming "near" our solar system in not too long.
 
Refining The Transit Timing And Photometric Analysis Of TRAPPIST-1: Masses, Radii, Densities, Dynamics, And Ephemerides - Astrobiology
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[2010.01074] Refining the transit timing and photometric analysis of TRAPPIST-1: Masses, radii, densities, dynamics, and ephemerides at ArXiv

They used an impressive sequence of observations over four years with several space-based and ground-based telescopes.

Total transits observed: 447, by planet 160, 107, 53, 49, 34, 30, 14.

Of these, 57 were observed with more than one telescope, making the total number of transit observations 504.

The orbit parameters are very similar to what was found earlier, but the masses are different.
  • b ... 1.017 +0.154 -0.143 ... 1.3771 +- 0.0593 ... 1.374 +- 0.069
  • c ... 1.156 .+0.142 -0.131 ... 1.3105 +- 0.0453 ... 1.308 +- 0.056
  • d ... 0.297 +0.039 -0.035 ... 0.3885 +- 0.0074 ... 0.388 +- 0.012
  • e ... 0.772 +0.079 -0.075 ... 0.6932 +- 0.0128 ... 0.692 +- 0.022
  • f ... 0.934 +0.080 -0.078 ... 1.0411 +- 0.0155 ... 1.039 +- 0.031
  • g ... 1.148 +0.098 -0.095 ... 1.3238 +- 0.0171 ... 1.321 +- 0.038
  • h ... 0.331 +0.056 -0.049 ... 0.3261 +- 0.0186 ... 0.326 +- 0.020
The pattern of masses and radii may be consistent with a uniform planetary composition for all seven planets which have lower uncompressed densities than the Earth, Mars or Venus, with weaker evidence for a declining normalized density with orbital period (88% confidence). The planet properties may either be consistent with a core mass fraction of 21±4 wt%, or an Earth-like core and mantle with a surface water content which varies from <0.001% for the inner three planets to ≈5% for the outer four, or core-free planets with highly oxidized iron in the mantle which elevates the interior light element content. These are not unique explanations.
There is also no evidence of an eighth planet with size similar to these planets and orbiting not very far from these planets.

Finally, I'll repeat my proposal of calling the star Adamski and its planets Orthon, Kalna, Ilmuth, Firkon, Ramu, Zuhl, and Charlotte.
 
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