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

Kepler's First Law of Planetary Motion01:10

Kepler's First Law of Planetary Motion

4.0K
In the early 17th century, German astronomer and mathematician Johannes Kepler postulated three laws for the motion of planets in the solar system. He formulated his first two laws based on the observations of his forebears, Nikolaus Copernicus and Tycho Brahe.
Polish astronomer Nikolaus Copernicus put forth a theory that stated a heliocentric model for the solar system. According to this heliocentric theory, all the planets, including Earth, orbit the Sun in circular orbits.
On the other hand,...
4.0K
Kepler's Third Law of Planetary Motion01:18

Kepler's Third Law of Planetary Motion

3.3K
In the early 17th century, German astronomer and mathematician Johannes Kepler postulated three laws for the motion of planets in the solar system. In 1909, he formulated his first two laws based on the observations of his forebears, Nikolaus Copernicus and Tycho Brahe. However, in 1918, he published his third law of planetary motion, which gives a precise mathematical relationship between a planet's average distance from the Sun and the amount of time it takes to revolve around the Sun. It...
3.3K
Kepler's Second Law of Planetary Motion01:29

Kepler's Second Law of Planetary Motion

4.2K
In the early 17th century, German astronomer and mathematician Johannes Kepler postulated three laws for the motion of planets in the solar system. His first law states that all planets orbit the Sun in an elliptical orbit, with the Sun at one of the ellipse's foci. Therefore, the distance of a planet from the Sun varies throughout its revolution around the Sun.
While in an elliptical orbit, the total energy of the planet is conserved. Therefore, the planet slows down when it is at apogee and...
4.2K
Schwarzschild Radius and Event Horizon01:21

Schwarzschild Radius and Event Horizon

2.0K
No object with a finite mass can travel faster than the speed of light in a vacuum. This fact has an interesting consequence in the domain of extremely high gravitational fields.
The minimum speed required to launch a projectile from the surface of an object to which it is gravitationally bound so that it eventually escapes the object’s gravitational field is called the escape velocity. The escape velocity is independent of the mass of the object. Merging the idea of escape...
2.0K
Circular Orbits and Critical Velocity for Satellites01:16

Circular Orbits and Critical Velocity for Satellites

2.9K
The Moon orbits around the Earth. In turn, the Earth (and other planets) orbit the Sun. The space directly above our atmosphere is filled with artificial satellites in orbit. One can examine the circular orbit, the simplest kind of orbit, to understand the relationship between the speed and the period of planets and satellites with respect to their positions and the bodies that they orbit.
Nicolaus Copernicus (1473-1543) first suggested that the Earth and all other planets orbit the Sun in...
2.9K
Reduced Mass Coordinates: Isolated Two-body Problem01:12

Reduced Mass Coordinates: Isolated Two-body Problem

1.3K
In classical mechanics, the two-body problem is one of the fundamental problems describing the motion of two interacting bodies under gravity or any other central force. When considering the motion of two bodies, one of the most important concepts is the reduced mass coordinates, a quantity that allows the two-body problem to be solved like a single-body problem. In these circumstances, it is assumed that a single body with reduced mass revolves around another body fixed in a position with an...
1.3K

You might also read

Related Articles

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

Sort by
Same author

The occupational therapy role in acute psychiatric inpatient units in Australia: A mixed methods study.

Australian occupational therapy journal·2026
Same author

Impact of Perfusion With Methylene Blue on Perioperative Bleeding in Simultaneous Pancreas and Kidney Transplantation: A Randomized Control Trial.

Transplantation direct·2026
Same author

The impact of the COVID-19 pandemic on admissions to an adolescent inpatient psychiatric unit.

Australasian psychiatry : bulletin of Royal Australian and New Zealand College of Psychiatrists·2026
Same author

Constraining an exoplanet's magnetic field using star-planet interactions.

Science (New York, N.Y.)·2026
Same author

Promoting Zinc Plating and Silencing the Hydrogen Evolution Reaction through Spatial Decoupling for Durable Aqueous Zinc-Ion Batteries.

ACS nano·2026
Same author

Lost in the system: lived experiences of eating disorder service models in Australia.

Journal of eating disorders·2026

Related Experiment Video

Updated: Jun 20, 2025

Simulation of the Planetary Interior Differentiation Processes in the Laboratory
06:04

Simulation of the Planetary Interior Differentiation Processes in the Laboratory

Published on: November 15, 2013

11.5K

A hot-Jupiter progenitor on a super-eccentric retrograde orbit.

Arvind F Gupta1,2,3, Sarah C Millholland4,5, Haedam Im4,5

  • 1U.S. National Science Foundation National Optical-Infrared Astronomy Research Laboratory (NSF NOIRLab), Tucson, AZ, USA. arvind.gupta@noirlab.edu.

Nature
|July 17, 2024
PubMed
Summary

Giant exoplanets, or hot Jupiters, likely migrate inward. This study found a high-mass, eccentric exoplanet, supporting the high-eccentricity tidal-migration pathway for hot Jupiter formation.

More Related Videos

Laboratory Drop Towers for the Experimental Simulation of Dust-aggregate Collisions in the Early Solar System
09:44

Laboratory Drop Towers for the Experimental Simulation of Dust-aggregate Collisions in the Early Solar System

Published on: June 5, 2014

12.7K
Surface Mapping of Earth-like Exoplanets using Single Point Light Curves
06:48

Surface Mapping of Earth-like Exoplanets using Single Point Light Curves

Published on: May 10, 2020

3.5K

Related Experiment Videos

Last Updated: Jun 20, 2025

Simulation of the Planetary Interior Differentiation Processes in the Laboratory
06:04

Simulation of the Planetary Interior Differentiation Processes in the Laboratory

Published on: November 15, 2013

11.5K
Laboratory Drop Towers for the Experimental Simulation of Dust-aggregate Collisions in the Early Solar System
09:44

Laboratory Drop Towers for the Experimental Simulation of Dust-aggregate Collisions in the Early Solar System

Published on: June 5, 2014

12.7K
Surface Mapping of Earth-like Exoplanets using Single Point Light Curves
06:48

Surface Mapping of Earth-like Exoplanets using Single Point Light Curves

Published on: May 10, 2020

3.5K

Area of Science:

  • Exoplanetary Science
  • Stellar and Galactic Astronomy
  • Planetary Dynamics

Background:

  • Giant exoplanets close to their stars (hot Jupiters) are unlikely to form in situ.
  • Migration from beyond the ice line is a leading theory, with high-eccentricity tidal migration proposed.
  • The exoplanet HD 80606 b provided initial evidence for this pathway, but similar progenitors are scarce.

Purpose of the Study:

  • To investigate the formation pathways of hot Jupiters.
  • To test the high-eccentricity tidal-migration hypothesis by searching for suitable exoplanet progenitors.
  • To analyze the relationship between exoplanet mass, eccentricity, and migration dynamics.

Main Methods:

  • Spectroscopic and photometric observations of exoplanets.
  • Analysis of orbital parameters, including eccentricity and mass.
  • Statistical analysis of the transiting warm-Jupiter population.

Main Results:

  • Discovery and characterization of TIC 241249530 b, a high-mass transiting warm Jupiter with extreme eccentricity (e=0.94).
  • The orbit of TIC 241249530 b is consistent with inward migration via eccentricity oscillations and future tidal circularization.
  • A correlation between high mass and high eccentricity was found in the transiting warm-Jupiter population.

Conclusions:

  • The findings support the high-eccentricity tidal-migration pathway as a viable mechanism for forming hot Jupiters.
  • Exoplanet mass is a critical factor in the efficacy of this migration channel, with high-mass planets being more likely to survive.
  • The observed correlation suggests that high-mass planets may preferentially undergo such extreme migration events.