Video Experimental Relacionado
Updated: Aug 12, 2026
09:38
Characterizing Far-infrared Laser Emissions and the Measurement of Their Frequencies
Published on: December 18, 2015
Señales de radiofrecuencia en la atmósfera de Júpiter
1L. J. Lanzerotti, Bell Laboratories, Lucent Technologies, Murray Hill, NJ 07974, and the University of Florida, Gainesville, FL 32611, USA. K. Rinnert, Max-Planck-Institut fur Aeronomy, D-37191 Katlenburg-Lindau, Germany. G. Dehmel, F. O. Gliem, J. Bach, Universitat Braunschweig, D-38106 Braunschweig, Germany. E. P. Krider, University of Arizona, Tucson, AZ 85721, USA. M. A. Uman, University of Florida, Gainesville, FL 32611, USA.
Science (New York, N.Y.)
|May 10, 1996
Resumen
La sonda Galileo detectó señales de radio significativas en la atmósfera de Júpiter, indicando regiones que no soportan rayos. La atmósfera de Júpiter se vuelve cada vez más opaca a presiones superiores a 4 bares.
Área de la Ciencia:
- Ciencias planetarias Ciencias planetarias.
- Física de la atmósfera Física de la atmósfera
- La radioastronomía es una radioastronomía.
Sus antecedentes:
- La sonda Galileo descendió a la atmósfera de Júpiter, equipada para medir las señales de radiofrecuencia.
- La comprensión previa de la composición atmosférica y la actividad eléctrica de Júpiter era limitada.
Objetivo del estudio:
- Para medir las señales de radiofrecuencia durante el descenso de la sonda Galileo.
- Para investigar la presencia y las características del rayo y la opacidad atmosférica en la atmósfera de Júpiter.
Principales métodos:
- Utilizando el detector de rayos y emisiones de radio a bordo de la sonda Galileo.
- Analizar las señales de radiofrecuencia a 3 y 15 kilohertz.
- La medición de la intensidad de la señal, las direcciones de llegada y las formas de onda en varios niveles de presión atmosférica.
Principales resultados:
- Se detectaron señales de radiofrecuencia significativamente por encima del ruido de fondo.
- Las intensidades de la señal variaban con la profundidad, disminuyendo a un nivel de presión de 5 bares antes de aumentar.
- La sonda atravesó una región aparentemente desprovista de rayos, lo que sugiere que la opacidad atmosférica aumenta bruscamente por encima de 4 bares.
Conclusiones:
- La atmósfera de Júpiter exhibe un comportamiento complejo de radiofrecuencia.
- La opacidad de la atmósfera joviana aumenta significativamente a presiones mayores de aproximadamente 4 bares.
- Los hallazgos proporcionan información sobre los procesos eléctricos y la estructura de la atmósfera profunda de Júpiter.
Videos de Conceptos Relacionados
02:37The Electromagnetic Spectrum
The electromagnetic spectrum consists of all the types of electromagnetic radiation arranged according to their frequency and wavelength. Each of the various colors of visible light has specific frequencies and wavelengths associated with them, and you can see that visible light makes up only a small portion of the electromagnetic spectrum. Because the technologies developed to work in various parts of the electromagnetic spectrum are different, for reasons of convenience and historical...
01:24IR Frequency Region: X–H Stretching
In IR spectroscopy, signals produced by the X−H bonds (such as C−H, O−H, or N−H) can be observed in the frequency range of 2700–4000 cm–1. The C−H stretching vibration forms sharp bands in the region 2850–3000 cm–1. The presence of the O−H stretching vibration leads to the forming of an absorption band in the frequency range 3650–3200 cm−1. At the same time, N−H stretching can be confirmed by absorption bands in the 3500–3100 cm−1 range. Even though both O−H and N−H bonds vibrate at a similar...
01:03IR Frequency Region: Fingerprint Region
IR spectra are divided into two main regions: the diagnostic region and the fingerprint region. The diagnostic region of the spectrum lies above 1500 cm−1. The absorptions resulting from single-bond vibrations of the N–H, C–H, and O–H stretch at higher wavenumbers and appear on the left side of the spectrum. The stretching absorptions of the C≡C and C≡N occur between 2100–2300 cm−1. In contrast, those arising from stretching absorptions of the C=O, C=N, and C=C occur between 1600–1850 cm−1.
The...
The...
01:30Electromagnetic Waves
James Clerk Maxwell formulated a single theory combining all the electric and magnetic effects scientists knew during that time, calling the phenomena his theory predicted “Electromagnetic waves”. He brought together all the work that had been done by brilliant physicists such as Oersted, Coulomb, Gauss, and Faraday and added his own insights to develop the overarching theory of electromagnetism. Maxwell’s equations, combined with the Lorentz force law, encompass all the laws of electricity and...
01:10Generating Electromagnetic Radiations
The German physicist Heinrich Hertz (1857–1894) was the first to generate and detect certain types of electromagnetic waves in the laboratory. Starting in 1887, he performed a series of experiments that confirmed the existence of electromagnetic waves and verified that they travel at the speed of light. Hertz used an alternating-current RLC (resistor-inductor-capacitor) circuit that resonated at a known frequency and connected it to a loop of wire. High voltages induced across the gap in the...
01:24The Electromagnetic Spectrum
Electromagnetic waves are categorized according to their wavelengths and frequencies, giving the electromagnetic spectrum. These waves are classified as radio, infrared, ultraviolet, etc. Radio waves refer to electromagnetic radiation with wavelengths ranging from millimeters to kilometers. Radio waves are commonly used for audio communications (i.e., radios) and typically result from an alternating current in the wires of a broadcast antenna. They cover a broad wavelength range and are used...