Jove
Visualize
Contact Us
JoVE
x logofacebook logolinkedin logoyoutube logo
ABOUT JoVE
OverviewLeadershipBlogJoVE Help Center
AUTHORS
Publishing ProcessEditorial BoardScope & PoliciesPeer ReviewFAQSubmit
LIBRARIANS
TestimonialsSubscriptionsAccessResourcesLibrary Advisory BoardFAQ
RESEARCH
JoVE JournalMethods CollectionsJoVE Encyclopedia of ExperimentsArchive
EDUCATION
JoVE CoreJoVE BusinessJoVE Science EducationJoVE Lab ManualFaculty Resource CenterFaculty Site
Terms & Conditions of Use
Privacy Policy
Policies

Related Concept Videos

Tidal Forces01:06

Tidal Forces

2.5K
The origin of Earth's ocean tides has been a subject of continuous investigation for over 2000 years. However, the work of Newton is considered to be the beginning of the proper understanding of the phenomenon. Ocean tides are the result of gravitational tidal forces. These same tidal forces are present in any astronomical body; they are responsible for the internal heat that creates the volcanic activity on Io, one of Jupiter's moons, and the breakup of stars that get too close to...
2.5K
Atomic Nuclei: Types of Nuclear Relaxation01:28

Atomic Nuclei: Types of Nuclear Relaxation

239
Nuclear relaxation restores the equilibrium population imbalance and can occur via spin–lattice or spin–spin mechanisms, which are first-order exponential decay processes.
In spin–lattice or longitudinal relaxation, the excited spins exchange energy with the surrounding lattice as they return to the lower energy level. Among several mechanisms that contribute to spin–lattice relaxation, magnetic dipolar interactions are significant. Here, the excited nucleus transfers...
239
Torsional Pendulum01:09

Torsional Pendulum

5.3K
A torsional pendulum involves the oscillation of a rigid body in which the restoring force is provided by the torsion in the string from which the rigid body is suspended. Ideally, the string should be massless; practically, its mass is much smaller than the rigid body's mass and is neglected.
As long as the rigid body's angular displacement is small, its oscillation can be modeled as a linear angular oscillation. The amplitude of the oscillation is an angle. The role of mass is played...
5.3K
Atomic Nuclei: Nuclear Relaxation Processes01:23

Atomic Nuclei: Nuclear Relaxation Processes

603
In the absence of an external magnetic field, nuclear spin states are degenerate and randomly oriented. When a magnetic field is applied, the spins begin to precess and orient themselves along (lower energy) or against (higher energy) the direction of the field. At equilibrium, a slight excess population of spins exists in the lower energy state. Because the direction of the magnetic field is fixed as the z-axis,  the precessing magnetic moments are randomly oriented around the z-axis.
603
Atomic Nuclei: Nuclear Spin State Population Distribution01:14

Atomic Nuclei: Nuclear Spin State Population Distribution

918
Near absolute zero temperatures, in the presence of a magnetic field, the majority of nuclei prefer the lower energy spin-up state to the higher energy spin-down state. As temperatures increase, the energy from thermal collisions distributes the spins more equally between the two states. The Boltzmann distribution equation gives the ratio of the number of spins predicted in the spin −½ (N−) and spin +½ (N+) states.
918
Spin–Spin Coupling Constant: Overview01:08

Spin–Spin Coupling Constant: Overview

863
In bromoethane, the three methyl protons are coupled to the two methylene protons that are three bonds away. In accordance with the n+1 rule, the signal from the methyl protons is split into three peaks with 1:2:1 relative intensities. The methylene protons appear as a quartet, with the relative intensities of 1:3:3:1.
Qualitatively, any spin plus-half nucleus polarizes the spins of its electrons to the minus-half state. Consequently, the paired electron in the hydrogen–carbon bond must...
863

You might also read

Related Articles

Articles linked to this work by shared authors, journal, and citation graph.

Sort by
Same author

Titan's strong tidal dissipation precludes a subsurface ocean.

Nature·2025
Same author

Endogenic heat at Enceladus' north pole.

Science advances·2025
Same author

Thermal asymmetry in the Moon's mantle inferred from monthly tidal response.

Nature·2025
Same author

Tidally driven remelting around 4.35 billion years ago indicates the Moon is old.

Nature·2024
Same author

Io's tidal response precludes a shallow magma ocean.

Nature·2024
Same author

Dual-frequency electromagnetic sounding of a Triton ocean from a single flyby.

Philosophical transactions. Series A, Mathematical, physical, and engineering sciences·2024

Related Experiment Video

Updated: May 29, 2025

Magnetically Induced Rotating Rayleigh-Taylor Instability
06:42

Magnetically Induced Rotating Rayleigh-Taylor Instability

Published on: March 3, 2017

9.5K

Titan's spin state as a constraint on tidal dissipation.

Brynna G Downey1,2, Francis Nimmo2

  • 1Southwest Research Institute, Boulder, CO 80302, USA.

Science Advances
|February 5, 2025
PubMed
Summary

Titan

Area of Science:

  • Planetary Science
  • Geophysics
  • Astrophysics

Background:

  • Tidal dissipation influences satellite orbital and rotational evolution.
  • Measuring dissipation rates (k2/Q) is challenging, with data limited to the Moon and Io.
  • Titan's unique characteristics may offer insights into satellite interiors.

Purpose of the Study:

  • To infer Titan's tidal dissipation parameters (k2/Q and K/Cs) using its rotational state.
  • To understand the implications of Titan's dissipation for its interior structure and evolution.
  • To establish a method for determining dissipation parameters for other icy moons.

Main Methods:

  • Analyzing Titan's observed deviation from its expected rotation.
  • Modeling tidal dissipation with varying ocean and ice shell thicknesses.

More Related Videos

Magnetic Tweezers for the Measurement of Twist and Torque
11:41

Magnetic Tweezers for the Measurement of Twist and Torque

Published on: May 19, 2014

23.2K
Methods for Measuring the Orientation and Rotation Rate of 3D-printed Particles in Turbulence
12:34

Methods for Measuring the Orientation and Rotation Rate of 3D-printed Particles in Turbulence

Published on: June 24, 2016

10.0K

Related Experiment Videos

Last Updated: May 29, 2025

Magnetically Induced Rotating Rayleigh-Taylor Instability
06:42

Magnetically Induced Rotating Rayleigh-Taylor Instability

Published on: March 3, 2017

9.5K
Magnetic Tweezers for the Measurement of Twist and Torque
11:41

Magnetic Tweezers for the Measurement of Twist and Torque

Published on: May 19, 2014

23.2K
Methods for Measuring the Orientation and Rotation Rate of 3D-printed Particles in Turbulence
12:34

Methods for Measuring the Orientation and Rotation Rate of 3D-printed Particles in Turbulence

Published on: June 24, 2016

10.0K
  • Calculating the tidal dissipation parameter (k2/Q) and boundary layer dissipation (K/Cs).

    • Main Results:

    • Inferred K/Cs range from 6.3 × 10^-14 to 2.4 × 10^-10 s^-1.
    • Inferred k2/Q ranges from 0.058 to 0.12, with a minimum Q ≈ 5.
    • Titan's dissipation parameters are significantly larger than the Moon's, suggesting a low effective viscosity.

    Conclusions:

    • Titan's high dissipation rate indicates rapid damping of its orbital eccentricity and inclination.
    • The findings suggest Titan's interior has a low effective viscosity.
    • Future missions like Dragonfly and JUICE can leverage this approach to study Titan and Ganymede.