Jove
Visualize
Contáctanos
JoVE
x logofacebook logolinkedin logoyoutube logo
ACERCA DE JoVE
Visión GeneralLiderazgoBlogCentro de Ayuda JoVE
AUTORES
Proceso de PublicaciónConsejo EditorialAlcance y PolíticasRevisión por ParesPreguntas FrecuentesEnviar
BIBLIOTECARIOS
TestimoniosSuscripcionesAccesoRecursosConsejo Asesor de BibliotecasPreguntas Frecuentes
INVESTIGACIÓN
JoVE JournalMethods CollectionsJoVE Encyclopedia of ExperimentsArchivo
EDUCACIÓN
JoVE CoreJoVE BusinessJoVE Science EducationJoVE Lab ManualCentro de Recursos para ProfesoresSitio de Profesores
Términos y Condiciones de Uso
Política de Privacidad
Políticas

Videos de Conceptos Relacionados

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
Energy of a Satellite in a Circular Orbit01:11

Energy of a Satellite in a Circular Orbit

2.3K
Thousands of artificial satellites orbit the Earth every day at various distances from the Earth. Satellites that orbit the Earth below an altitude of 1,600 km are considered to be orbiting in low-Earth orbit (LEO). Research satellites and Earth observation satellites are usually placed in LEO, and mostly orbit the Earth in elliptical orbits. Navigation satellites are placed in medium-Earth orbit (MEO), ranging from 2,000 km to 36,000 km from the surface of the Earth. Meanwhile, communication...
2.3K
Kepler's Third Law of Planetary Motion01:18

Kepler's Third Law of Planetary Motion

3.4K
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...
3.4K
Kepler's Second Law of Planetary Motion01:29

Kepler's Second Law of Planetary Motion

4.3K
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...
4.3K
Kepler's First Law of Planetary Motion01:10

Kepler's First Law of Planetary Motion

4.1K
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,...
4.1K
Schwarzschild Radius and Event Horizon01:21

Schwarzschild Radius and Event Horizon

2.1K
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...
2.1K

También podría leer

Artículos Relacionados

Artículos vinculados a este trabajo por autores compartidos, revista y gráfico de citas.

Ordenar por
Same author

A sudden change and recovery in the magnetic environment around a repeating fast radio burst.

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

Detection of disk-jet coprecession in a tidal disruption event.

Science advances·2025
Same author

Starspots as the origin of ultrafast drifting radio bursts from an active M dwarf.

Science advances·2025
Same author

Quasi-periodic oscillations of GHz-band polarization in a black hole.

Nature communications·2025
Same author

Discovery of a high-velocity cloud of the Milky Way as a potential dark galaxy.

Science advances·2025
Same author

Magnetar emergence in a peculiar gamma-ray burst from a compact star merger.

National science review·2025

Video Experimental Relacionado

Updated: Jul 26, 2025

Bringing the Visible Universe into Focus with Robo-AO
10:35

Bringing the Visible Universe into Focus with Robo-AO

Published on: February 12, 2013

19.5K

Un púlsar binario en una órbita de 53 minutos

Z Pan1,2,3,4, J G Lu1,2,3,4, P Jiang5,6,7,8

  • 1National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China.

Nature
|June 20, 2023
PubMed
Resumen
Este resumen es generado por máquina.

Los investigadores descubrieron un nuevo púlsar araña, PSR J1953+1844 (M71E), con un período orbital inusualmente corto y un compañero de baja masa. Este hallazgo ayuda a cerrar la brecha entre los diferentes tipos de púlsares y comprender su evolución.

Más Videos Relacionados

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

3.6K
3D Orbital Tracking in a Modified Two-photon Microscope: An Application to the Tracking of Intracellular Vesicles
11:28

3D Orbital Tracking in a Modified Two-photon Microscope: An Application to the Tracking of Intracellular Vesicles

Published on: October 1, 2014

10.3K

Videos de Experimentos Relacionados

Last Updated: Jul 26, 2025

Bringing the Visible Universe into Focus with Robo-AO
10:35

Bringing the Visible Universe into Focus with Robo-AO

Published on: February 12, 2013

19.5K
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

3.6K
3D Orbital Tracking in a Modified Two-photon Microscope: An Application to the Tracking of Intracellular Vesicles
11:28

3D Orbital Tracking in a Modified Two-photon Microscope: An Application to the Tracking of Intracellular Vesicles

Published on: October 1, 2014

10.3K

Área de la Ciencia:

  • * Astronomía y astrofísica
  • * Física de objetos compactos
  • * Sistemas de estrellas binarias

Sus antecedentes:

  • * Los púlsares araña son estrellas de neutrones con estrellas compañeras cercanas, lo que lleva a períodos de rotación de milisegundos y órbitas cortas.
  • * Estos sistemas son cruciales para comprender la evolución de los púlsares, los efectos de la irradiación y la formación de estrellas de neutrones.
  • * Los púlsares viudas negras tienen compañeros de muy baja masa, que potencialmente evolucionaron de los púlsares redback.

Objetivo del estudio:

  • * Para buscar y caracterizar púlsares de milisegundos con compañeros de masa moderada y períodos orbitales muy cortos.
  • * Para investigar el vínculo evolutivo entre diferentes tipos de púlsares.
  • * Para informar del descubrimiento de un nuevo sistema binario de pulsares de milisegundos.

Principales métodos:

  • * Observaciones por radio del púlsar binario de milisegundos PSR J1953+1844 (M71E).
  • * Análisis del período orbital y la masa de la estrella compañera.
  • * Detección y localización de la fuente de rayos X.

Principales resultados:

  • * El descubrimiento de PSR J1953+1844 (M71E), un púlsar binario de milisegundos.
  • * Período orbital de 53,3 minutos.
  • * La estrella compañera tiene una masa de aproximadamente 0,07 M.
  • * Situado cerca del centro del cúmulo globular M71.

Conclusiones:

  • * El sistema descubierto llena un vacío en la población esperada de púlsares.
  • * Proporciona nuevos conocimientos sobre la evolución de los púlsares araña y sus compañeros.
  • * Contribuye a la comprensión de la diversidad de las binarias de estrellas de neutrones.