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

Conditions on Early Earth02:06

Conditions on Early Earth

Around 4 billion years ago, oceans began to condense on earth while volcanic eruptions released nitrogen, carbon dioxide, methane, ammonia, and hydrogen into the primordial atmosphere. However, organisms with the characteristics of life were not initially present on earth. Scientists have used experimentation to determine how organisms evolved that could grow, reproduce, and maintain an internal environment.
Conditions on Early Earth02:06

Conditions on Early Earth

Around 4 billion years ago, oceans began to condense on earth while volcanic eruptions released nitrogen, carbon dioxide, methane, ammonia, and hydrogen into the primordial atmosphere. However, organisms with the characteristics of life were not initially present on earth. Scientists have used experimentation to determine how organisms evolved that could grow, reproduce, and maintain an internal environment.
Kepler's First Law of Planetary Motion01:10

Kepler's First Law of Planetary Motion

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,...
Kepler's Second Law of Planetary Motion01:29

Kepler's Second Law of Planetary Motion

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...
Kepler's Third Law of Planetary Motion01:18

Kepler's Third Law of Planetary Motion

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...
Design Example: Calculating Safe Diameter for Wind-Exposed Disc01:17

Design Example: Calculating Safe Diameter for Wind-Exposed Disc

Assessing safety in wind-exposed installations is crucial to preventing potential failures. This example explores the calculation and design adjustments needed to mount a circular disc on a building facade, where wind forces are a primary concern. A 4-meter diameter disc was initially designed as an aesthetic feature facing winds at a velocity of 25 meters per second, with an air density of 1.25 kilograms per cubic meter. Given these conditions, the drag force on the disc was determined using...

You might also read

Related Articles

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

Sort by
Same author

Accretion bursts crystallize silicates in a planet-forming disk.

Nature·2026
Same author

From Hardship to Harmony: Life Reviews of Korean American Immigrants Assisted by Companion Robots.

Research on aging·2025
Same author

Emission lines due to ionizing radiation from a compact object in the remnant of Supernova 1987A.

Science (New York, N.Y.)·2024
Same author

Factors Associated with Person-Centered Care among Hospice Nurses.

Journal of hospice and palliative care·2023
Same author

Neural cell adhesion molecule 1 is a cellular target engaged plasma biomarker in demyelinating Charcot-Marie-Tooth disease.

European journal of neurology·2023
Same author

Combining remote sensing analysis with machine learning to evaluate short-term coastal evolution trend in the shoreline of Venice.

The Science of the total environment·2022

Related Experiment Video

Updated: May 9, 2026

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 16, 2013

The development of a protoplanetary disk from its natal envelope.

Dan M Watson1, C J Bohac, C Hull

  • 1Department of Physics and Astronomy, University of Rochester, Rochester, New York 14627-0171, USA. dmw@pas.rochester.edu

Nature
|August 31, 2007
PubMed
Summary

Astronomers observed water emission from the young protostar NGC 1333-IRAS 4B, revealing details of a forming protoplanetary disk. This finding offers insights into the early stages of planet formation around young stellar objects.

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

Scattering And Absorption of Light in Planetary Regoliths
11:34

Scattering And Absorption of Light in Planetary Regoliths

Published on: July 1, 2019

Related Experiment Videos

Last Updated: May 9, 2026

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 16, 2013

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

Scattering And Absorption of Light in Planetary Regoliths
11:34

Scattering And Absorption of Light in Planetary Regoliths

Published on: July 1, 2019

Area of Science:

  • Astronomy and Astrophysics
  • Star Formation and Evolution
  • Exoplanetary Science

Background:

  • Class 0 protostars are the earliest stage of young stellar objects, crucial for understanding protoplanetary disk formation.
  • Previous studies indicated warmer, denser regions within protostars like NGC 1333-IRAS 4, but lacked detailed observation.
  • Millimeter-wavelength observations have shown kinematic signatures of collapse in protostellar envelopes.

Purpose of the Study:

  • To investigate the core structure of the proto-multiple system NGC 1333-IRAS 4 on Solar System scales.
  • To detect and analyze the composition of gas within the embedded region of a Class 0 protostar.
  • To observe the early development of a protoplanetary disk.

Main Methods:

  • Mid-infrared observations (20-37 micrometers) of NGC 1333-IRAS 4B.
  • Analysis of molecular line emission, specifically water (H2O).
  • Modeling of observed emission to infer gas properties and infall dynamics.

Main Results:

  • Detection of a rich H2O emission spectrum from NGC 1333-IRAS 4B.
  • The emission originates from extremely dense and warm gas.
  • The data supports a model of infall onto a deeply embedded, dense disk, indicating protoplanetary disk development.
  • This is the only Class 0 object in a sample of 30 to show such mid-infrared water emission.

Conclusions:

  • The observations provide direct evidence of a forming protoplanetary disk around a Class 0 protostar.
  • The unique detection may be due to favorable orientation or represent a transient evolutionary phase.
  • This study offers a rare glimpse into the critical early stages of planet formation.