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Tidal locking

Tidal locking, also known as synchronous rotation, is a gravitational phenomenon where the rotation period of a celestial body becomes synchronized with its orbital period around a larger partner, causing one side of the body to consistently face the partner.^[1] This synchronization arises from tidal forces that distort the smaller body's shape into bulges, with friction from these deforming bulges dissipating rotational energy as heat, gradually slowing the rotation until it matches the orbital rate.^[2] In the Solar System, all large moons, such as Earth's Moon and the major satellites of Jupiter and Saturn, are tidally locked to their parent planets, a process that typically occurs early in their formation, often within hundreds of thousands of years for larger bodies.^[1] Notable exceptions include mutual tidal locking, as seen in the Pluto-Charon system, where both bodies face each other perpetually.^[1] This effect extends beyond moons to some exoplanets orbiting close to their stars and certain binary star systems, influencing planetary climates, geological activity, and potential habitability by stabilizing or altering rotational dynamics.^[1] For Earth's Moon, tidal locking resulted from initial rapid rotation following its formation from a massive collision, with ongoing tidal interactions causing it to recede from Earth at about 4 centimeters per year.^[1] Over billions of years, such forces may eventually lead to Earth becoming tidally locked to the Moon as well.^[1]

Fundamentals

Definition and Principles

Tidal locking occurs in a gravitationally bound system when the rotation period of a smaller body matches its orbital period around a larger primary body, ensuring that one hemisphere of the smaller body consistently faces the primary.^[1] This synchronization results from long-term gravitational interactions that stabilize the rotational state over time.^[3] Key characteristics of tidal locking include synchronous rotation, where the smaller body's spin aligns precisely with its orbital motion, establishing a 1:1 spin-orbit resonance.^[4] This resonance leads to a permanent division of the smaller body's surface into a dayside perpetually illuminated by the primary and a nightside in constant shadow, with transitional regions experiencing prolonged twilight.^[1] Such configurations are common among natural satellites and close-orbiting planets due to the stabilizing influence of gravitational torques.^[5] The term "tidal locking" derives from the tidal forces generated by the gravitational gradient between the bodies, which drive the rotational synchronization.^[3] This effect was first systematically described by astronomer Giovanni Domenico Cassini in 1693 through observations of the Moon, where he formulated laws including its synchronous rotation relative to Earth.^[6] A simple illustration of tidal locking typically depicts a moon orbiting a planet with the same facial features—such as craters or markings—always oriented toward the planet, emphasizing the fixed orientation.^[1]

Physical Basis

Tidal locking arises from the interaction between gravitational forces and the rotational dynamics of celestial bodies, where tides serve as the primary mechanism driving the synchronization of rotation and orbital motion. The physical foundation lies in the gravitational gradient, which refers to the variation in gravitational acceleration across an extended body due to a nearby massive object. This differential pull stretches the body into a prolate spheroid shape, elongating it along the line connecting the centers of the two bodies. For instance, the Moon's gravity creates such a gradient on Earth, leading to ocean bulges, while on solid bodies like planets, it deforms the crust and mantle.^[7] The magnitude of the tidal force responsible for this deformation is given by the approximation F \propto \frac{G M m r}{d^3}, where G is the gravitational constant, M is the mass of the perturbing body, m is the mass of the test particle within the deformed body, r is the distance from the center of the deformed body to the particle, and d is the separation between the centers of the two bodies. This force arises from the difference in gravitational attraction on points at slightly different distances from the perturber, resulting in a tidal acceleration that scales inversely with the cube of the distance d. The r/d^3 dependence highlights how the effect is strongest near the perturber and diminishes rapidly with distance, making it significant only for close-orbiting bodies.^[8]^[7] In the absence of rotation, the body assumes an equilibrium tide configuration, where the deformation matches the instantaneous gravitational potential of the perturber, forming static bulges aligned with the line of centers. However, when the body rotates, these bulges become dynamic tides, oscillating and potentially lagging or leading the equilibrium position due to the body's inertia, elasticity, and internal friction. This distinction is crucial, as dynamic tides introduce time-varying stresses that facilitate energy dissipation and angular momentum transfer.^[9] The process of tidal locking involves spin-orbit coupling, governed by the conservation of total angular momentum in the system, which includes both the orbital angular momentum and the spin angular momentum of the bodies. As tides transfer angular momentum from the body's rotation to its orbit (or vice versa), the total remains constant, leading to a gradual alignment of the rotation period with the orbital period. This conservation principle underpins the long-term evolution toward synchronization observed in many binary systems.^[10]

Mechanism

Tidal Bulge Formation

Tidal forces arise from the differential gravitational attraction exerted by a primary body on a satellite, causing the satellite to deform into an elongated shape. This deformation manifests as two tidal bulges: the near-side bulge, where the satellite's material is pulled toward the primary by the stronger gravitational field on the closer side, and the far-side bulge, resulting from the weaker pull on the distant side combined with the centrifugal force due to the satellite's orbital motion around the system's center of mass.^[11] The equilibrium shape for a fluid body would align these bulges perfectly along the line connecting the centers of the two bodies, but real bodies exhibit partial rigidity that limits the deformation.^[12] When the satellite's rotation rate differs from its orbital angular velocity, the tidal bulges do not remain aligned with this line of centers. Instead, internal material response delays the bulges, creating a misalignment that generates a gravitational torque. This torque acts on the satellite's rotation and the primary's orbit, with the magnitude depending on the offset angle between the bulges and the line of centers.^[1] The degree of deformation is quantified by the second-degree tidal Love number k_2, which measures the ratio of the body's tidal potential perturbation to the perturbing tidal potential and reflects its rigidity; values of k_2 range from 1.5 for fluid bodies to much smaller for highly rigid ones.^[13] Energy dissipation during deformation is characterized by the tidal quality factor Q, which indicates the ratio of stored to dissipated energy in the tidal response, with higher Q implying less friction. The resulting bulge lag angle \delta \theta, which drives the torque, arises from internal friction within the satellite, modeled as a viscoelastic material response, where deformational energy is converted to heat through hysteresis in the material's strain cycle. The dissipation rate is proportional to k_2 / Q, highlighting how both rigidity and frictional properties influence the efficiency of energy loss.

Synchronization Process

The synchronization process in tidal locking arises from tidal torques generated by the gravitational interaction between two bodies, where friction within the tidally deformed body causes a lag in the alignment of the tidal bulge relative to the line connecting the centers of mass. This misalignment results in a net torque as the primary body gravitationally pulls on the lagged bulge, transferring angular momentum from the body's rotational kinetic energy to its orbital motion (or vice versa, depending on the initial configuration).^[14] The direction of the torque opposes the relative motion between the rotation and orbit, driving the system toward equilibrium where the rotational period matches the orbital period.^[15] For a satellite in prograde rotation initially faster than its orbital rate around a more massive primary, the tidal torque systematically decelerates the spin, reducing the rotation rate until synchronization is achieved, at which point the torque vanishes and the bulge aligns perfectly with the primary. This process conserves total angular momentum while dissipating rotational energy as heat through internal friction.^[16] In systems where the masses of the two bodies are comparable, tidal torques act on both, potentially leading to mutual locking where both rotations synchronize with the orbital period. The rate of change of the rotation rate \Omega for the tidally deformed body in such equilibrium evolution is given by

\dot{\Omega} = -\frac{3 G M^2 k_2 R^5}{Q I \alpha^6},

where G is the gravitational constant, M the mass of the primary, k_2 the second-degree tidal Love number, R the radius of the deformed body, Q the tidal dissipation factor, I the moment of inertia of the deformed body, and \alpha the orbital separation.^[17] In the case of eccentric orbits, full synchronization to the mean orbital period may not occur; instead, a pseudo-synchronous rotation state can emerge, where the average tidal torque over one orbit is zero, typically resulting in a rotation rate slightly faster than the mean motion to balance the varying gravitational forces.^[18] This equilibrium minimizes energy dissipation while maintaining a stable configuration distinct from true synchronous locking.

Orbital Modifications

Tidal interactions in a two-body system generate torques that transfer angular momentum between the rotational states of the bodies and their mutual orbit. When dissipation occurs primarily in the more massive primary, the torque accelerates the primary's rotation or transfers angular momentum from its spin to the orbit, leading to orbital expansion. Conversely, if the mass ratio favors significant dissipation in the less massive secondary, the torque can extract angular momentum from the orbit, causing contraction. This behavior depends on the relative strengths of tidal dissipation in each body, with the direction of migration reversing based on which component dominates the energy loss.^[15] A key orbital modification is the damping of eccentricity due to tidal friction, which circularizes the orbit over time. The rate of eccentricity change is described by the relation \frac{de}{dt} \propto -\frac{e}{(1 - e^2)^{13/2}}, where e is the orbital eccentricity; this form arises from the equilibrium tide model and highlights how damping accelerates for higher initial eccentricities until the orbit approaches circularity.^[18] The net migration of the secondary depends on the locus of dissipation: outward migration occurs when the primary's tides dominate, as angular momentum is added to the orbit, while inward migration results if the secondary's internal friction prevails, drawing angular momentum from the orbit to spin up the secondary. This dichotomy explains diverse evolutionary paths in planetary systems, such as the outward drift of Jupiter's Galilean satellites driven by Jupiter's dissipation.^[19] In certain scenarios, particularly for bodies with specific mass ratios or initial conditions, full 1:1 tidal locking may not be achieved; instead, the system can stabilize in a 2:1 spin-orbit resonance, where the secondary completes two rotations per orbital period, serving as an alternative equilibrium state.^[20]

Timescales

Influencing Factors

The rate of tidal dissipation within a satellite fundamentally governs the speed of tidal locking, as it determines how quickly angular momentum is transferred between the satellite's rotation and orbit. This dissipation is quantified by the tidal quality factor Q, defined as the ratio of the peak stored tidal energy to the energy dissipated per radian of oscillation; lower Q values indicate more efficient energy loss as heat, accelerating synchronization.^[21] For instance, Q typically ranges from 10 to 100 near material melting points, where viscoelastic relaxation enhances friction.^[21] The satellite's composition and internal structure further modulate Q: rocky bodies generally exhibit higher Q (around 100–280, reflecting greater rigidity) compared to icy bodies, which have lower Q (often 10–100) due to the more dissipative nature of ice under tidal straining.^[22]^[23] In layered structures, such as those with a fluid core or mantle, dissipation concentrates in deformable interfaces, potentially lowering effective Q by orders of magnitude.^[24] The strength of the tidal torque, which drives the locking process, scales strongly with the mass ratio between primary and satellite, as well as their separation. Specifically, the torque \Gamma is proportional to \frac{M_p^2 R_s^5}{a^6}, where M_p is the primary's mass, R_s the satellite's radius, and a the semi-major axis; thus, more massive primaries and closer orbits (smaller a) produce stronger torques, hastening locking.^[17] This dependence arises because tidal forces, varying as M_p / a^3, raise larger bulges on bigger satellites (R_s), amplifying the gravitational misalignment that generates torque.^[17] Satellites orbiting massive stars or gas giants, like those around Jupiter, therefore lock more rapidly than those around less massive hosts.^[19] Initial rotational and orbital conditions also shape the locking outcome and timescale. A satellite starting with rapid spin (e.g., near breakup speed from formation) requires longer to despin to synchrony, as the initial angular momentum deficit is greater, though the torque remains constant.^[25] Orbital eccentricity influences the equilibrium state: low-eccentricity orbits favor 1:1 spin-orbit resonance, while higher eccentricity can trap the satellite in non-synchronous resonances (e.g., 3:2), altering the final rotational period.^[25] Environmental features like atmospheres or subsurface oceans can boost dissipation beyond solid-body contributions. Dense atmospheres generate thermal tides, where solar heating creates pressure waves that interact with planetary rotation, adding frictional losses and effectively reducing Q.^[26] Similarly, subsurface oceans in icy satellites enhance tidal response by decoupling the rigid ice shell from the core, allowing greater bulge deformation and resonance-enhanced energy dissipation in the fluid layer.^[27] These effects are pronounced in ocean worlds like Europa, where ocean tides contribute significantly to total heating.^[24]

Estimation Techniques

Estimation of tidal locking timescales relies on balancing the tidal torque with the angular momentum of the body's rotation. The analytical timescale \tau for synchronization is derived by equating the rate of change of rotational angular momentum to the tidal torque, yielding \tau \approx \frac{2 Q I \Omega}{3 G M_p^2 k_2 R_s^5} a^6, where Q is the tidal quality factor, I is the moment of inertia, \Omega is the initial rotation rate, G is the gravitational constant, M_p is the primary's mass, k_2 is the tidal Love number, R_s is the satellite's radius, and a is the semi-major axis. This formula assumes constant dissipation and provides order-of-magnitude estimates for systems where tidal forces dominate. Numerical simulations extend these analytical models by incorporating variable dissipation and complex orbital dynamics using N-body integrators. Early foundations trace to George Darwin's 19th-century viscous sphere theory, which modeled tidal bulges and friction but assumed constant viscosity. Modern updates integrate realistic rheology models, such as viscoelastic responses in icy or rocky bodies, allowing for frequency-dependent Q values that vary with rotation and orbital periods.^[28] Tools like RheoVolution employ these in N-body frameworks to simulate long-term evolution, capturing non-linear effects like resonance capture that analytical approximations overlook.^[28] Approaches differ in handling the phase lag between tidal bulges and the perturbing body: constant-phase-lag (CPL) models assume a fixed lag angle, simplifying to a constant Q for quick estimates but ignoring material-dependent dissipation.^[29] In contrast, constant-time-lag (CTL) or time-dependent phase lag models account for realistic varying dissipation by incorporating frequency dependence, better suiting bodies with complex interiors like planets with oceans or partial melts.^[29] These are essential for accurate predictions in systems with evolving eccentricities. Recent advancements incorporate machine learning to accelerate predictions of tidal locking in exoplanet systems, training on simulation outputs to estimate timescales from orbital parameters without full N-body runs. Post-2020 studies apply neural networks to model tidal evolution in star-planet interactions, enabling rapid assessment for large catalogs of close-in exoplanets.^[30] This approach enhances efficiency for habitability assessments by forecasting locking probabilities under uncertain dissipation parameters.^[30]

Occurrence

In the Solar System

In the Solar System, tidal locking is a common phenomenon among the major regular satellites of the outer planets, where gravitational interactions with their parent bodies have synchronized their rotations to match their orbital periods. All large moons of Jupiter, Saturn, Uranus, and Neptune exhibit this synchronous rotation, always keeping the same hemisphere facing their planet. This includes Jupiter's Galilean moons—Io, Europa, Ganymede, and Callisto—which orbit close enough for tidal forces to enforce locking over billions of years. Similarly, Saturn's major inner moons, such as Mimas, Enceladus, Tethys, Dione, Rhea, and especially Titan, are tidally locked, as are Uranus's five principal moons (Miranda, Ariel, Umbriel, Titania, and Oberon) and Neptune's Triton, the latter despite its captured origin from the Kuiper Belt.^[1]^[31]^[32] A striking example of mutual tidal locking involves the Pluto-Charon binary system, where both the dwarf planet Pluto and its large moon Charon are synchronously rotated relative to each other, orbiting a common barycenter outside Pluto's radius. This configuration results from strong tidal interactions that have circularized their orbit and aligned their rotations. Data from NASA's New Horizons flyby in July 2015 provided detailed confirmation of this mutual locking, revealing consistent surface features on the facing hemispheres and supporting models of their tidal evolution.^[33]^[34] The innermost planet, Mercury, demonstrates a stable but non-synchronous form of tidal locking known as a 3:2 spin-orbit resonance, in which it rotates three times on its axis for every two revolutions around the Sun. This resonance arose from chaotic early orbital dynamics influenced by Venus and Jupiter, capturing Mercury into this configuration approximately 3-4 billion years ago and preventing full 1:1 locking due to its greater distance from the Sun compared to typical locked moons. Irregular satellites, such as the distant, retrograde outer moons of Jupiter, Saturn, Uranus, and Neptune (e.g., Phoebe around Saturn), are generally not tidally locked because their wide, eccentric, and inclined orbits result in weaker and more variable tidal torques, insufficient for synchronization over the Solar System's age. NASA's observations indicate that while all gravitationally rounded large moons are locked, these smaller, captured bodies often retain asynchronous rotations due to their dynamical instability. Potential tidal locking has also been inferred for some small Kuiper Belt objects, particularly in binary pairs, where close separations enable rapid tidal evolution toward synchrony, as modeled in systems like those observed by New Horizons.^[1]^[35]

In Extrasolar Systems

Hot Jupiters, massive gas giant exoplanets orbiting very close to their host stars with periods typically under 3 days, experience strong tidal forces that lead to near-universal tidal locking, where the planet's rotation period matches its orbital period. This synchronization occurs on timescales of less than a billion years, far shorter than the age of most systems, making it a standard outcome for these planets. For instance, HD 189733 b, a prototypical hot Jupiter with an orbital period of 2.2 days, shows a rotation period consistent with synchronous locking based on high-resolution spectroscopy measurements. Analyses of data from the Kepler and TESS missions support this, with theoretical models indicating that nearly all hot Jupiters with periods shorter than 3 days are tidally locked, as the tidal locking timescale is much shorter than the typical age of their host stars.^[36] Earth-sized rocky exoplanets in the habitable zones of cool M-dwarf stars are also prone to tidal locking owing to their proximity to the host star, which places them within the regime where tidal torques dominate over billions of years. The TRAPPIST-1 system, discovered in 2017, exemplifies this phenomenon: its seven terrestrial planets, with orbital periods from 1.5 to 19 days, are all likely tidally locked, resulting in permanent daysides and nightsides that influence their climates and potential atmospheres. Such configurations are common for small planets around low-mass stars, as tidal equilibrium is reached efficiently due to the stars' weak magnetic braking and the planets' close-in orbits.^[37]^[38] In binary star systems beyond the Solar System, tidal locking manifests as synchronized rotations between the components, particularly in close pairs where gravitational interactions are intense. Contact binaries, in which the stars' Roche lobes overflow and they share a common convective envelope, routinely exhibit rotational periods equal to their orbital periods, a direct result of tidal friction dissipating angular momentum differences. RS CVn-type binaries, characterized by chromospheric activity and evolved components, similarly show tidal synchronization, with rotation periods matching orbital ones in short-period systems (typically under 20 days), enhancing their magnetic dynamo activity. Brown dwarfs in wide binaries or circumbinary configurations can also achieve locking, as seen in systems where their rotation aligns with orbital motion over gigayear timescales.^[39]^[40] Recent James Webb Space Telescope (JWST) observations since 2022 have illuminated tidal locking in white dwarf binary systems, revealing synchronized dynamics in post-main-sequence pairs. For example, in eclipsing white dwarf-brown dwarf binaries like WD 0137-349B, the secondary is inferred to be tidally locked, with its rotation period equaling the ~2-hour orbital period, as deduced from photometric and spectroscopic data showing stable light curves consistent with synchronous rotation. These findings, spanning 2022–2025 campaigns, highlight how tidal forces maintain locking even in degenerate remnants, influencing mass transfer and evolutionary paths.^[41] Tidal locking in extrasolar systems is detected indirectly through methods that probe rotational and orbital dynamics. Radial velocity (RV) measurements, often combined with the Rossiter-McLaughlin effect during transits, can indicate spin-orbit alignment, a hallmark of locking by revealing low stellar obliquities in systems with close-in planets. Transit timing variations (TTVs), observed in multi-planet setups like those from Kepler and TESS, signal gravitational perturbations that arise from tidal resonances, indirectly supporting spin synchronization by demonstrating orbital stability influenced by tidal dissipation. These techniques have confirmed locking in select cases, such as resonant chains where TTVs align with expected tidal equilibria.^[42]^[43]

Implications

Dynamical Effects

Tidal locking contributes to the orbital stability of locked bodies by minimizing tidal torques that could otherwise drive perturbations in spin and orbit. In such configurations, the synchronous rotation aligns the body's rotational bulge with the line connecting it to the primary, reducing dissipative forces and making the system more resistant to external gravitational disturbances from nearby bodies. This stability is particularly evident in hierarchical systems, where the locked state helps maintain long-term orbital coherence.^[44] In multi-moon systems around a planet, tidal interactions often drive the alignment of satellite orbits with the Laplace plane, an invariant plane determined by the balance of the planet's equatorial bulge and the central star's perturbation. This alignment enhances overall dynamical stability by confining orbital inclinations and preventing chaotic scattering among the moons. For instance, during the Laplace plane transition, tidal dissipation can reorient orbits toward this stable plane, avoiding instabilities that might otherwise lead to moon loss or collisions.^[45] Cassini states represent equilibrium configurations in tidally locked systems where the spin axis, orbital pole, and the primary's equatorial pole align in a specific geometry, balancing precessional torques. These states arise from the interplay of tidal friction and orbital perturbations, resulting in a fixed obliquity \theta relative to the orbital inclination I. For the primary Cassini state (state 1), the equilibrium condition is given by

\frac{\sin(I - \theta)}{\sin \theta} = -\frac{3}{2} \frac{C - A}{C} \cos I,

where C and A are the body's polar and equatorial moments of inertia, respectively. This equation, derived from averaged Hamiltonian dynamics, describes how the obliquity adjusts to maintain the alignment, with the spin axis precessing at the same rate as the orbit. Such equilibria are common in locked satellites like the Moon, ensuring long-term axial stability despite secular perturbations. In binary systems exhibiting mutual tidal locking, such as Pluto and Charon, both bodies synchronize their rotations to the mutual orbital period, which circularizes and expands the orbit while stabilizing the configuration against perturbations. This dual locking transfers angular momentum efficiently from spins to the orbit, damping eccentricities and inclinations over timescales of 1–10 million years, thereby preventing close encounters that could destabilize the system. The resulting near-circular orbit resists further tidal evolution, maintaining a robust equilibrium. However, tidally locked systems with high orbital eccentricities face significant disruption risks, as varying tidal forces can induce chaotic spin evolution or orbital instabilities. Elevated eccentricity amplifies tidal dissipation episodically during periastron passages, potentially exciting resonances that lead to tumbling or mode instabilities in the locked body. In extreme cases, this chaos can culminate in ejection from the system or tidal disruption if the orbit decays sufficiently, particularly in multi-body environments where perturbations exacerbate the eccentricity.^[46]

Observational and Habitability Impacts

Tidal locking produces distinctive observational signatures that aid in characterizing exoplanets. Thermal phase curves, observed through broadband photometry or spectroscopy, exhibit a pronounced day-night contrast, with peak emission from the permanently illuminated substellar hemisphere and minimal output from the darkside, reflecting limited heat redistribution in thin atmospheres.^[47] Transmission spectroscopy during transits primarily samples the terminator zones—the twilight boundaries between day and night—revealing atmospheric compositions and potential haze layers that differ from dayside or nightside profiles.^[48] These features enable differentiation of tidally locked worlds from non-synchronous rotators, as the fixed orientation amplifies hemispheric asymmetries in emitted flux.^[49] On tidally locked planets, extreme climates often manifest as the "eyeball" effect, where intense stellar heating confines liquid water to a circular region around the substellar point, while the surrounding land freezes and the antistellar hemisphere becomes uninhabitable.^[50] Atmospheric circulation, driven by day-night temperature gradients, can partially mitigate this by transporting heat equatorward and toward the nightside via winds, potentially expanding the liquid water zone beyond the substellar area.^[50] For Proxima Centauri b, 2016 general circulation models demonstrated that efficient heat transport in a thick atmosphere could sustain global habitability, with surface temperatures averaging 250–300 K even under modest greenhouse effects.^[51] Habitability faces significant challenges from the asynchronous exposure to stellar radiation on M-dwarf planets, where the dayside endures elevated UV fluxes from frequent flares, risking atmospheric erosion, ozone depletion, and DNA damage to surface life.^[52] Global oceans, however, offer a counterbalance by enabling efficient meridional and longitudinal heat redistribution through currents, which can homogenize temperatures and support subsurface or polar habitats less affected by irradiation.^[53] This oceanic transport broadens the effective habitable zone, allowing liquid water stability across larger fractions of the surface compared to land-dominated worlds.^[54] Simulations from 2022–2025 highlight mechanisms enhancing habitability in locked systems, such as tidally induced volcanic activity that drives plate tectonics and the carbon-silicate cycle, maintaining long-term liquid water via CO₂ regulation.^[55] Models of ocean-bearing planets show substellar "lone seas"—isolated water bodies at the dayside center—fostering nutrient upwelling and microbial ecosystems, with sporadic rotation episodes further promoting circulation to avert full freeze-overs.^[56] Additionally, 2025 studies on mantle convection reveal that perpetual stellar forcing sustains internal heating, potentially fueling cryovolcanism on icy ocean worlds and expanding subsurface habitability.^[57] Recent 2024–2025 research further indicates that while stellar winds may erode atmospheres on tidally locked exoplanets orbiting active stars, night-side regions could maintain stable liquid water, potentially extending habitability beyond the substellar point.^[58]^[59] These findings underscore how geological and hydrological feedbacks can transform tidal locking from a barrier into an enabler for life.^[60]

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Feb 8, 2021 · Most hot Jupiters have typical orbital periods of ∼3 days. For in-situ formation, we expect hot Jupiters to be located at or beyond the disk ...
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TRAPPIST-1 is Older Than Our Solar System - NASA Science
Aug 11, 2017 · All seven planets are likely tidally locked to their star, each with a perpetual dayside and nightside. At the time of its discovery, scientists ...
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Tidal heating and the habitability of the TRAPPIST-1 exoplanets
Tidal forces raise and lower a bulge on each planet; as the height of the bulge changes, the planet does work against its own internal rigidity resulting in the ...
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A study of X-ray flares – II. RS CVn-type binaries - Oxford Academic
The high activity level of RS CVns is generally due to their fast rotation, itself a consequence of tidal locking of the stellar rotation period with the ...
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XMM-Newton's view of a RS CVn binary CF Tuc - ScienceDirect.com
In short period RS CVns, the two stars are locked due to tidal forces i.e. the rotational period is equal to the orbital period of the binary (for more details ...
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The only inflated brown dwarf in an eclipsing white dwarf–brown ...
2022; Brown et al. 2023). The brown dwarfs in these systems are likely tidally locked, as hot Jupiters are, and the irradiation of the brown dwarf results in ...
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Rossiter-McLaughlin detection of the 9-month period transiting ...
The HARPS-N data reveal a jump in radial velocity within the night at the expected time of the transit egress with a difference of 3.4 ± 1.1 m s−1.
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Investigating Transit Timing Variations in the Ultrashort Period ...
Jul 31, 2025 · In this study, we present a comprehensive analysis of transit timing variations (TTVs) in the ultrashort-period gas giant WASP-19b, which orbits ...
[44]
stability of tidal equilibrium for hierarchical star–planet–moon systems
In contrast, Pluto and Charon and mutually tidally locked. The rotational periods of Pluto and Charon, as well as their orbital period, are all about 6.4 d.
[45]
[PDF] Tidal Friction in the Earth-Moon System and Laplace Planes
Apr 16, 2015 · ... Love number and lag angle can be written k20 sin δ20. Thus if (46) and (47) are divided by (48), then those equations become. 1. JM. dJM da. = 1.
[46]
Tidal Evolution and Diffusive Growth During High-eccentricity Planet ...
High-eccentricity tidal migration is a potential formation channel for hot Jupiters. During this process, the planetary f-mode may experience a phase of ...
[47]
DECIPHERING THERMAL PHASE CURVES OF DRY, TIDALLY ...
We investigate which atmospheric properties can, and cannot, be inferred from the broadband thermal phase curve of a dry and tidally locked terrestrial planet.Missing: zones | Show results with:zones
[48]
[PDF] Exoplanetary Atmospheres: Key Insights, Challenges and Prospects
Transit spectroscopy allows observations of transmission spectra of day-night ter- minator, thermal emission spectra of dayside, and phase curves over the orbit ...<|separator|>
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[PDF] arXiv:1412.8216v1 [astro-ph.EP] 28 Dec 2014
Dec 28, 2014 · For a tidally locked planet the phase curve depends largely on the at- mospheric redistribution of energy between day- side and nightside. Many ...
[50]
The habitability of Proxima Centauri b - II. Possible climates and ...
On a tidally locked planet with sufficient surface water inventory, liquid water is always present, at least in the substellar region. With a non-synchronous ...
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[PDF] Exploring the climate of Proxima B with the Met Office Unified Model
Aug 24, 2018 · We present results of simulations of the climate of the newly discovered planet Proxima Centauri B, performed using the Met Office.
[52]
The Surface UV Environment on Planets Orbiting M Dwarfs
Most habitability studies of M dwarfs treat UV radiation as a negative for habitability (Heath et al. ... tidally locked habitable-zone M-dwarf planets.
[53]
Habitability and sub glacial liquid water on planets of M-dwarf stars
Apr 14, 2023 · As demonstrated below, considering tidally locked planets of M-dwarfs ... On the bio-habitability of M-dwarf planets. Astrophys. J. 858, 1 ...
[54]
On the Biohabitability of M-dwarf Planets - IOPscience
On the Biohabitability of M-dwarf Planets. A. Wandel ... Planets within the HZ of M dwarfs are often close enough to their hosts to be tidally locked.
[55]
Tidally driven tectonic activity as a parameter in exoplanet habitability
Tidally driven tectonic activity, like plate tectonics on Earth, may help maintain surface liquid water on exoplanets by supporting the long-term carbon cycle.Missing: lone | Show results with:lone
[56]
[PDF] Habitability of Tidally Locked Planets with Sporadic Rotation - arXiv
Jul 14, 2023 · Planets that orbit close to their stars are typically assumed to be tidally locked due to increased tidal forces and dissipation. In ...
[57]
Convective dynamics in mantle of tidally-locked exoplanets - Nature
Jul 25, 2025 · However, tidally-locked exoplanets may maintain vigorous convection as they keep large Θ due to the perpetual exposure to the stellar flux.Missing: lone | Show results with:lone
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Prospects for Cryovolcanic Activity on Cold Ocean Planets
Oct 4, 2023 · We have estimated total internal heating rates and depths to possible subsurface oceans for 17 planets that may be cold ocean planets.<|control11|><|separator|>