adsabs/AstroCLIMB huggingface dataset:
Paper: Direct Imaging Explorations for Companions around Mid–Late M Stars from the Subaru/IRD Strategic Program 
Authors: Taichi Uyama, Charles Beichman, Masayuki Kuzuhara, Markus Janson, Takayuki Kotani, Dimitri Mawet, Bun'ei Sato, Motohide Tamura, Hiroyuki Tako Ishikawa, Bryson Cale, Thayne Currie, Hiroki Harakawa, Thomas Henning, Teruyuki Hirano, Klaus Hodapp, Yasunori Hori, Masato Ishizuka, Shane Jacobson, Yui Kasagi, Eiichiro Kokubo, Mihoko Konishi, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Jungmi Kwon, Masahiro Machida, Takao Nakagawa, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Ji Wang
Figure caption: Summary of the Subaru/IRD-FIM images that resolved companions. The target name is labeled in the upper right corner of each panel. All images are rotated such that north is up and the primary star is located at the center. The color scale is arbitrarily set to clearly show our detections.
Paper: Direct Imaging Explorations for Companions around Mid–Late M Stars from the Subaru/IRD Strategic Program 
Authors: Taichi Uyama, Charles Beichman, Masayuki Kuzuhara, Markus Janson, Takayuki Kotani, Dimitri Mawet, Bun'ei Sato, Motohide Tamura, Hiroyuki Tako Ishikawa, Bryson Cale, Thayne Currie, Hiroki Harakawa, Thomas Henning, Teruyuki Hirano, Klaus Hodapp, Yasunori Hori, Masato Ishizuka, Shane Jacobson, Yui Kasagi, Eiichiro Kokubo, Mihoko Konishi, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Jungmi Kwon, Masahiro Machida, Takao Nakagawa, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Ji Wang
Figure caption: Left: 5σ contrast limit of the postprocessed ﹩L^{\prime} ﹩-band data in our observations. We utilized RDI for the LSPM J0044+0907 data set and ADI for the other data sets. We also present the detected companions from the NIRC2 ﹩L^{\prime} ﹩-band observations (LSPM J0825+6902 B, LSPM J1645+0444 B, and LSPM J2204+1505 B), indicated by red circles. Right: converted mass limit from the contrast limit overlaid with the detected companions as shown in the left panel and the COND03 evolutionary model assuming 1 and 10 Gyr.
Paper: TOI-1695 b: A Water World Orbiting an Early-M Dwarf in the Planet Radius Valley
Authors: Collin Cherubim, Ryan Cloutier, David Charbonneau, Chris Stockdale, Keivan G. Stassun, Richard P. Schwarz, Boris Safonov, Annelies Mortier, Pablo Lewin, David W. Latham, Keith Horne, Raphaëlle D. Haywood, Erica Gonzales, Maria V. Goliguzova, Karen A. Collins, David R. Ciardi, Allyson Bieryla, Alexandre A. Belinski, Bill Wohler, Christopher A. Watson, Roland Vanderspek, Stéphane Udry, Alessandro Sozzetti, Damien Ségransan, Dimitar Sasselov, George R. Ricker, Ken Rice, Ennio Poretti, Giampaolo Piotto, Francesco Pepe, Emilio Molinari, Giuseppina Micela, Michel Mayor, Christophe Lovis, Mercedes López-Morales, Jon M. Jenkins, Zahra Essack, Xavier Dumusque, John P. Doty, Knicole D. Colón, Andrew Collier Cameron, Lars A. Buchhave
Figure caption: TESS PDCSAP light curve of TOI-1695 from Sectors 18, 19, 24, 25, and 52. Top row: the dilution-, systematic-, and background-corrected PDCSAP light curves overlaid with our mean GP model of the residual correlated noise (pink curve). Middle row: the PDCSAP light curve detrended after subtraction of our mean GP model. In-transit measurements are highlighted in red. Bottom panel: the phase-folded transit light curve of TOI-1695 b with 24 minute bins. The maximum a posteriori transit model is overlaid in red and the white markers depict the binned light curve.
Paper: TOI-1695 b: A Water World Orbiting an Early-M Dwarf in the Planet Radius Valley
Authors: Collin Cherubim, Ryan Cloutier, David Charbonneau, Chris Stockdale, Keivan G. Stassun, Richard P. Schwarz, Boris Safonov, Annelies Mortier, Pablo Lewin, David W. Latham, Keith Horne, Raphaëlle D. Haywood, Erica Gonzales, Maria V. Goliguzova, Karen A. Collins, David R. Ciardi, Allyson Bieryla, Alexandre A. Belinski, Bill Wohler, Christopher A. Watson, Roland Vanderspek, Stéphane Udry, Alessandro Sozzetti, Damien Ségransan, Dimitar Sasselov, George R. Ricker, Ken Rice, Ennio Poretti, Giampaolo Piotto, Francesco Pepe, Emilio Molinari, Giuseppina Micela, Michel Mayor, Christophe Lovis, Mercedes López-Morales, Jon M. Jenkins, Zahra Essack, Xavier Dumusque, John P. Doty, Knicole D. Colón, Andrew Collier Cameron, Lars A. Buchhave
Figure caption: ASAS-SN photometric monitoring of TOI-1695. Top row: the full V-band photometric light curve over its four-year baseline, overplotted with our best-fit sinusoidal model of stellar rotation with an amplitude of 7.7 ppt. The marker colors indicate the epoch of each observation. The right panel depicts a GLS periodogram of the light curve and reveals a strong signal at 48 days. Middle row: the residual light curve after the removal of the best-fit stellar rotation model. The corresponding GLS periodogram reveals no significant residual periodicities. Bottom panel: the light curve and rotation model phase folded to the measured stellar rotation of 47.7 days.
Paper: TOI-1695 b: A Water World Orbiting an Early-M Dwarf in the Planet Radius Valley
Authors: Collin Cherubim, Ryan Cloutier, David Charbonneau, Chris Stockdale, Keivan G. Stassun, Richard P. Schwarz, Boris Safonov, Annelies Mortier, Pablo Lewin, David W. Latham, Keith Horne, Raphaëlle D. Haywood, Erica Gonzales, Maria V. Goliguzova, Karen A. Collins, David R. Ciardi, Allyson Bieryla, Alexandre A. Belinski, Bill Wohler, Christopher A. Watson, Roland Vanderspek, Stéphane Udry, Alessandro Sozzetti, Damien Ségransan, Dimitar Sasselov, George R. Ricker, Ken Rice, Ennio Poretti, Giampaolo Piotto, Francesco Pepe, Emilio Molinari, Giuseppina Micela, Michel Mayor, Christophe Lovis, Mercedes López-Morales, Jon M. Jenkins, Zahra Essack, Xavier Dumusque, John P. Doty, Knicole D. Colón, Andrew Collier Cameron, Lars A. Buchhave
Figure caption: Companion sensitivity from high-resolution imaging. Top: the results from Keck/NIRC2 AO imaging in the Br–γ filter. The black points represent the 5σ limits and are separated in steps of 1 FWHM (∼0.″054); the purple represents the azimuthal dispersion (1σ) of the contrast determinations. The inset image is of the primary target showing no additional companions to within 3″ of the target. Bottom: the results from SAI speckle polarimetry in the I  c  band. The black curve depicts the 5σ contrast limits and the inset shows the combined intensity image on a linear scale.
Paper: TOI-1695 b: A Water World Orbiting an Early-M Dwarf in the Planet Radius Valley
Authors: Collin Cherubim, Ryan Cloutier, David Charbonneau, Chris Stockdale, Keivan G. Stassun, Richard P. Schwarz, Boris Safonov, Annelies Mortier, Pablo Lewin, David W. Latham, Keith Horne, Raphaëlle D. Haywood, Erica Gonzales, Maria V. Goliguzova, Karen A. Collins, David R. Ciardi, Allyson Bieryla, Alexandre A. Belinski, Bill Wohler, Christopher A. Watson, Roland Vanderspek, Stéphane Udry, Alessandro Sozzetti, Damien Ségransan, Dimitar Sasselov, George R. Ricker, Ken Rice, Ennio Poretti, Giampaolo Piotto, Francesco Pepe, Emilio Molinari, Giuseppina Micela, Michel Mayor, Christophe Lovis, Mercedes López-Morales, Jon M. Jenkins, Zahra Essack, Xavier Dumusque, John P. Doty, Knicole D. Colón, Andrew Collier Cameron, Lars A. Buchhave
Figure caption: Ground-based transit light curves of TOI-1695.01 taken as part of TFOP. The solid curves depict the optimized transit model fits with all model parameters fixed other than the baseline flux, midtransit time, and planet-to-star radius ratio. Annotated next to each light curve is the telescope facility, passband of the observation, and UT observation date. Here we only depict the four light curves that were confirmed to have temporal coverage over a transit event.
Paper: TOI-1695 b: A Water World Orbiting an Early-M Dwarf in the Planet Radius Valley
Authors: Collin Cherubim, Ryan Cloutier, David Charbonneau, Chris Stockdale, Keivan G. Stassun, Richard P. Schwarz, Boris Safonov, Annelies Mortier, Pablo Lewin, David W. Latham, Keith Horne, Raphaëlle D. Haywood, Erica Gonzales, Maria V. Goliguzova, Karen A. Collins, David R. Ciardi, Allyson Bieryla, Alexandre A. Belinski, Bill Wohler, Christopher A. Watson, Roland Vanderspek, Stéphane Udry, Alessandro Sozzetti, Damien Ségransan, Dimitar Sasselov, George R. Ricker, Ken Rice, Ennio Poretti, Giampaolo Piotto, Francesco Pepe, Emilio Molinari, Giuseppina Micela, Michel Mayor, Christophe Lovis, Mercedes López-Morales, Jon M. Jenkins, Zahra Essack, Xavier Dumusque, John P. Doty, Knicole D. Colón, Andrew Collier Cameron, Lars A. Buchhave
Figure caption: Mass–radius diagram for small planets orbiting M dwarfs with masses measured to better than 3σ from the NASA Exoplanet Archive, including TOI-1695 b for comparison (large square). The planet marker shapes indicate the bulk composition interpretation as rocky (circles), gaseous (triangles), or intermediate (squares). The solid curves depict internal structure models with mass fractions of 100% water, 33% iron plus 67% rock (i.e., Earth-like), and 100% iron (Zeng & Sasselov 2013). The dashed curves depict models of Earth-like cores hosting H2 envelopes of varying mass fractions and equilibrium temperatures (Zeng et al. 2019). The shaded region corresponds to the forbidden region according to models of maximum collisional mantle stripping by giant impacts (Marcus et al. 2010). The seven keystone planets are bolded.
Paper: TOI-1695 b: A Water World Orbiting an Early-M Dwarf in the Planet Radius Valley
Authors: Collin Cherubim, Ryan Cloutier, David Charbonneau, Chris Stockdale, Keivan G. Stassun, Richard P. Schwarz, Boris Safonov, Annelies Mortier, Pablo Lewin, David W. Latham, Keith Horne, Raphaëlle D. Haywood, Erica Gonzales, Maria V. Goliguzova, Karen A. Collins, David R. Ciardi, Allyson Bieryla, Alexandre A. Belinski, Bill Wohler, Christopher A. Watson, Roland Vanderspek, Stéphane Udry, Alessandro Sozzetti, Damien Ségransan, Dimitar Sasselov, George R. Ricker, Ken Rice, Ennio Poretti, Giampaolo Piotto, Francesco Pepe, Emilio Molinari, Giuseppina Micela, Michel Mayor, Christophe Lovis, Mercedes López-Morales, Jon M. Jenkins, Zahra Essack, Xavier Dumusque, John P. Doty, Knicole D. Colón, Andrew Collier Cameron, Lars A. Buchhave
Figure caption: The TOI-1695 HARPS-N RVs and model components along with their corresponding GLS periodogram. Top row: the raw RVs. The vertical blue dashed line in the periodogram highlights the orbital period of TOI-1695 b while the red dashed lines highlight the stellar rotation period and its first harmonic. Second row: the activity component of our RV model (i.e., raw RVs minus the maximum a posteriori Keplerian model) overlaid with the mean GP model (red curve). The shaded region represents the standard deviation of the GP. Third row: the RV signal from TOI-1695 b overlaid with the maximum a posteriori Keplerian solution for TOI-1695 b (blue curve). Fourth row: the RV residuals. Bottom panel: the activity-corrected RVs phase folded to the orbital period of TOI-1695 b. The RV measurement uncertainties throughout include the contribution from the additive scalar jitter term s RV.(The data used to create this figure are available.)
Paper: TOI-1695 b: A Water World Orbiting an Early-M Dwarf in the Planet Radius Valley
Authors: Collin Cherubim, Ryan Cloutier, David Charbonneau, Chris Stockdale, Keivan G. Stassun, Richard P. Schwarz, Boris Safonov, Annelies Mortier, Pablo Lewin, David W. Latham, Keith Horne, Raphaëlle D. Haywood, Erica Gonzales, Maria V. Goliguzova, Karen A. Collins, David R. Ciardi, Allyson Bieryla, Alexandre A. Belinski, Bill Wohler, Christopher A. Watson, Roland Vanderspek, Stéphane Udry, Alessandro Sozzetti, Damien Ségransan, Dimitar Sasselov, George R. Ricker, Ken Rice, Ennio Poretti, Giampaolo Piotto, Francesco Pepe, Emilio Molinari, Giuseppina Micela, Michel Mayor, Christophe Lovis, Mercedes López-Morales, Jon M. Jenkins, Zahra Essack, Xavier Dumusque, John P. Doty, Knicole D. Colón, Andrew Collier Cameron, Lars A. Buchhave
Figure caption: Period–radius diagram for small planets transiting M dwarfs and with precisely measured RV masses (>3σ). The dashed lines depict model predictions of the location of the M dwarf radius valley from thermally driven mass loss and from gas depleted formation. The shaded wedge regions host the so-called keystone planets, including the newly discovered TOI-1695 b. The marker shapes depict planets whose bulk compositions have been determined to be Earth-like (circles), gas-rich (triangles), or intermediate (squares; see Section 5.1 for definitions). The color bar highlights each planet's incident instellation.
Paper: TOI-1695 b: A Water World Orbiting an Early-M Dwarf in the Planet Radius Valley
Authors: Collin Cherubim, Ryan Cloutier, David Charbonneau, Chris Stockdale, Keivan G. Stassun, Richard P. Schwarz, Boris Safonov, Annelies Mortier, Pablo Lewin, David W. Latham, Keith Horne, Raphaëlle D. Haywood, Erica Gonzales, Maria V. Goliguzova, Karen A. Collins, David R. Ciardi, Allyson Bieryla, Alexandre A. Belinski, Bill Wohler, Christopher A. Watson, Roland Vanderspek, Stéphane Udry, Alessandro Sozzetti, Damien Ségransan, Dimitar Sasselov, George R. Ricker, Ken Rice, Ennio Poretti, Giampaolo Piotto, Francesco Pepe, Emilio Molinari, Giuseppina Micela, Michel Mayor, Christophe Lovis, Mercedes López-Morales, Jon M. Jenkins, Zahra Essack, Xavier Dumusque, John P. Doty, Knicole D. Colón, Andrew Collier Cameron, Lars A. Buchhave
Figure caption: RV detection sensitivity to planets orbiting TOI-1695 as a function of planet mass and orbital period. The solid lines mark the 10% and 90% sensitivity limits, respectively. The circle marker highlights TOI-1695 b. Dotted red lines show constant semi-amplitudes of 1, 2.5, and 10 m s−1. The shaded region spans the HZ of TOI-1695 whose inner and outer edges are defined by the recent Venus and early Mars boundaries (Kopparapu et al. 2013).
Paper: TOI-1695 b: A Water World Orbiting an Early-M Dwarf in the Planet Radius Valley
Authors: Collin Cherubim, Ryan Cloutier, David Charbonneau, Chris Stockdale, Keivan G. Stassun, Richard P. Schwarz, Boris Safonov, Annelies Mortier, Pablo Lewin, David W. Latham, Keith Horne, Raphaëlle D. Haywood, Erica Gonzales, Maria V. Goliguzova, Karen A. Collins, David R. Ciardi, Allyson Bieryla, Alexandre A. Belinski, Bill Wohler, Christopher A. Watson, Roland Vanderspek, Stéphane Udry, Alessandro Sozzetti, Damien Ségransan, Dimitar Sasselov, George R. Ricker, Ken Rice, Ennio Poretti, Giampaolo Piotto, Francesco Pepe, Emilio Molinari, Giuseppina Micela, Michel Mayor, Christophe Lovis, Mercedes López-Morales, Jon M. Jenkins, Zahra Essack, Xavier Dumusque, John P. Doty, Knicole D. Colón, Andrew Collier Cameron, Lars A. Buchhave
Figure caption: The solid red line shows the stellar surface EUV flux evolution model used in the TOI-1695 b photoevaporation simulations (Section 5.2; Equation (8)). The dashed lines show the integrated flux density for 10 nm < λ < 130 nm from the HAZMAT synthetic spectra (Peacock et al. 2020). These spectra are computed for the lower quartile, median, and upper quartile EUV flux density samples of early-M dwarfs at five ages: 10, 45, 120, 650 Myr, and 5 Gyr. We chose F EUV,0 = 180 W m−2 for our model. Our EUV flux model is shown to be consistent with the semi-empirical data.
Paper: TOI-1695 b: A Water World Orbiting an Early-M Dwarf in the Planet Radius Valley
Authors: Collin Cherubim, Ryan Cloutier, David Charbonneau, Chris Stockdale, Keivan G. Stassun, Richard P. Schwarz, Boris Safonov, Annelies Mortier, Pablo Lewin, David W. Latham, Keith Horne, Raphaëlle D. Haywood, Erica Gonzales, Maria V. Goliguzova, Karen A. Collins, David R. Ciardi, Allyson Bieryla, Alexandre A. Belinski, Bill Wohler, Christopher A. Watson, Roland Vanderspek, Stéphane Udry, Alessandro Sozzetti, Damien Ségransan, Dimitar Sasselov, George R. Ricker, Ken Rice, Ennio Poretti, Giampaolo Piotto, Francesco Pepe, Emilio Molinari, Giuseppina Micela, Michel Mayor, Christophe Lovis, Mercedes López-Morales, Jon M. Jenkins, Zahra Essack, Xavier Dumusque, John P. Doty, Knicole D. Colón, Andrew Collier Cameron, Lars A. Buchhave
Figure caption: Results of our photoevaporation simulation, which models EUV-driven hydrodynamic escape and thermal contraction on TOI-1695 b. Each curve corresponds to a different initial envelope mass fraction. The planetary radius decreases to the observed radius (1.90 R ⊕) on megayear timescales, a making present-day H/He-enveloped rocky core an unlikely composition.
Paper: TOI-1695 b: A Water World Orbiting an Early-M Dwarf in the Planet Radius Valley
Authors: Collin Cherubim, Ryan Cloutier, David Charbonneau, Chris Stockdale, Keivan G. Stassun, Richard P. Schwarz, Boris Safonov, Annelies Mortier, Pablo Lewin, David W. Latham, Keith Horne, Raphaëlle D. Haywood, Erica Gonzales, Maria V. Goliguzova, Karen A. Collins, David R. Ciardi, Allyson Bieryla, Alexandre A. Belinski, Bill Wohler, Christopher A. Watson, Roland Vanderspek, Stéphane Udry, Alessandro Sozzetti, Damien Ségransan, Dimitar Sasselov, George R. Ricker, Ken Rice, Ennio Poretti, Giampaolo Piotto, Francesco Pepe, Emilio Molinari, Giuseppina Micela, Michel Mayor, Christophe Lovis, Mercedes López-Morales, Jon M. Jenkins, Zahra Essack, Xavier Dumusque, John P. Doty, Knicole D. Colón, Andrew Collier Cameron, Lars A. Buchhave
Figure caption: The SED and best-fit stellar atmosphere model of TOI-1695. The red markers depict the photometric measurements with horizontal error bars that depict the effective width of each passband. The black curve depicts the best-fit stellar atmosphere model with T eff = 3630 K. The blue circles depict the model fluxes integrated over each passband.
Paper: Tidal Heating of Exomoons in Resonance and Implications for Detection
Authors: Armen Tokadjian, Anthony L. Piro
Figure caption: A constant Hamiltonian curve for a planet orbited by a test-particle moon and perturbing moon in a 2:1 resonance. Here, Δ = 1 and K = 0.5. The x and y coordinates represent the canonical momentum and canonical coordinate, functions of semimajor axis and eccentricity that vary for all points except the fixed points. These are shown here in red at (−1, 0) and (2, 0).
Paper: Tidal Heating of Exomoons in Resonance and Implications for Detection
Authors: Armen Tokadjian, Anthony L. Piro
Figure caption: A constant Hamiltonian curve for the Jupiter–Io–Europa system. Here, Δ = −2.245 and K = −0.276. Because this system is in close to perfect resonance, there is little libration and the trajectory is a small circle. The minimum of the Hamiltonian, the fixed point, is the red point at (0.293, 0), which is in the center of the trajectory.
Paper: Tidal Heating of Exomoons in Resonance and Implications for Detection
Authors: Armen Tokadjian, Anthony L. Piro
Figure caption: Tidal heating luminosities and temperatures for two Io-like moons orbiting a planet in a 2:1 resonance. Each row corresponds to a different planet mass and each column refers to the orbital periods of the two moons in resonance. The red curves represent the tidal luminosity with the red horizontal line set at the average luminosity. The tidal heating temperature is shown by the orange curves, with the average temperature, the orange horizontal line, calculated using the average luminosity and displayed at the left corner of each plot. There is a clear trend of decreasing temperature as planet mass and orbital periods increase.
Paper: Tidal Heating of Exomoons in Resonance and Implications for Detection
Authors: Armen Tokadjian, Anthony L. Piro
Figure caption: Constant Hamiltonian phase curves of a planet orbited by two moons in resonance and zero initial eccentricity for simulation (left) and theory (right). Here, m  p /m 2 = 300 and the inner and outer moons have orbital periods of 2 days and 4 days, respectively. The trajectory shows that the eccentricity does not remain zero but oscillates along with semimajor axis. The fixed point is the red dot at (1.26, 0) and corresponds to the minimum of the Hamiltonian.
Paper: Tidal Heating of Exomoons in Resonance and Implications for Detection
Authors: Armen Tokadjian, Anthony L. Piro
Figure caption: Maximum orbital periods of exomoons around 25 rocky planets that can potentially retain a moon for over 300 Myr (brown) and 85 Neptune-like planets that can retain a moon for over 5 Gyr (blue). The smallest maximum moon period is 10 days and the largest is 90 days. This stability range allows for placement of moons in a variety of 2:1 orbital configurations, such as the 2 day/4 day periods we consider in this paper.
Paper: Tidal Heating of Exomoons in Resonance and Implications for Detection
Authors: Armen Tokadjian, Anthony L. Piro
Figure caption: Analysis of three properties of 30 exoplanets to distinguish potential exomoon detections through tidal heating. Each point traces T irr of the given planet plotted against the planet’s radius. The color corresponds to the distance from Earth, and filled circles are the planets with an available estimated mass. The solid vertical lines divide the planets by composition with rocky on the left and Neptune-like on the right, while the horizontal dashed lines represent the habitable zone.
Paper: Tidal Heating of Exomoons in Resonance and Implications for Detection
Authors: Armen Tokadjian, Anthony L. Piro
Figure caption: Tidal heating luminosity and temperature for the system described in Figure 3, where m  p  = 4.5 M ⊕. The horizontal red line shows the average luminosity from which the average temperature, the horizontal orange line, is calculated with T avg shown at the top left.
Paper: Tidal Heating of Exomoons in Resonance and Implications for Detection
Authors: Armen Tokadjian, Anthony L. Piro
Figure caption: Constant Hamiltonian trajectories and tidal heating curves for the Jupiter–Io–Europa system at varying eccentricities for Io’s orbit. The blue curve in each shows the changing semimajor axis and eccentricity of Io and the red dot is the fixed point where this variation is minimized. The red curves are the tidal luminosity generated in Io and the orange curves below are the corresponding tidal temperature. The system is in closest to perfect resonance at e = 0.005, where the blue circle is smallest and the luminosity varies the least.
Paper: Tidal Heating of Exomoons in Resonance and Implications for Detection
Authors: Armen Tokadjian, Anthony L. Piro
Figure caption: Inner moon eccentricity evolution over time for the system in Figure 3. The initially circular orbit grows in eccentricity and then oscillates with an amplitude of 0.1536 due to the system’s distance from the minimum of the Hamiltonian.
Paper: Tidal Heating of Exomoons in Resonance and Implications for Detection
Authors: Armen Tokadjian, Anthony L. Piro
Figure caption: Libration period vs. perturbing mass for the theoretical relation given by Equation (9), in blue, compared to simulation results, shown as red points. The mass of the planet is 1.37 M ⊕ and the eccentricity of the inner moon orbit is 0.094. The red curve is the best-fitting power law to the simulation results with a power-law index of 0.73.
Paper: Tidal Heating of Exomoons in Resonance and Implications for Detection
Authors: Armen Tokadjian, Anthony L. Piro
Figure caption: Similar to Figure 6 but for Io in the three-body system consisting of Jupiter, Io, and Europa. The average tidal heating temperature of Io is 92 K, which agrees with the upper bound set by observation.
Paper: Tidal Heating of Exomoons in Resonance and Implications for Detection
Authors: Armen Tokadjian, Anthony L. Piro
Figure caption: Blackbody curve for TOI-4353.01 and a theoretical Io-sized moon orbiting in a 2:1 resonance with an outer moon. In this case, the moon outshines the planet because of significant tidal heating, which makes this planet a good candidate for possible moon detection through the secondary eclipse method. At the wavelength where the moon’s curve peaks, the moon’s luminosity is more than 100 times the planet’s luminosity.