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The solar wind is a stream of charged particles released from the upper atmosphere of the Sun, called the corona. This plasma mostly consists of electrons, protons and alpha particles with kinetic energy between 0.5 and 10 keV. The composition of the solar wind plasma also includes a mixture of materials found in the solar plasma: trace amounts of heavy ions and atomic nuclei such as C, N, O, Ne, Mg, Si, S, and Fe. There are also rarer traces of some other nuclei and isotopes such as P, Ti, Cr, 54Fe and 56Fe, and 58Ni, 60Ni, and 62Ni. Superposed with the solar-wind plasma is the interplanetary magnetic field. The solar wind varies in density, temperature and speed over time and over solar latitude and longitude. Its particles can escape the Sun's gravity because of their high energy resulting from the high temperature of the corona, which in turn is a result of the coronal magnetic field. The boundary separating the corona from the solar wind is called the Alfvén surface.
The solar mass (M☉) is a standard unit of mass in astronomy, equal to approximately 2×1030 kg. It is often used to indicate the masses of other stars, as well as stellar clusters, nebulae, galaxies and black holes. It is approximately equal to the mass of the Sun. This equates to about two nonillion (short scale), two quintillion (long scale) kilograms or 2000 quettagrams:
A coronal mass ejection (CME) is a significant release of plasma and accompanying magnetic field from the Sun's corona into the heliosphere. CMEs are often associated with solar flares and other forms of solar activity, but a broadly accepted theoretical understanding of these relationships has not been established.
Eugene Newman Parker was an American solar and plasma physicist. In the 1950s he proposed the existence of the solar wind and that the magnetic field in the outer Solar System would be in the shape of a Parker spiral, predictions that were later confirmed by spacecraft measurements. In 1987, Parker proposed the existence of nanoflares, a leading candidate to explain the coronal heating problem.
A prominence, sometimes referred to as a filament, is a large plasma and magnetic field structure extending outward from the Sun's surface, often in a loop shape. Prominences are anchored to the Sun's surface in the photosphere, and extend outwards into the solar corona. While the corona consists of extremely hot plasma, prominences contain much cooler plasma, similar in composition to that of the chromosphere.
Solar physics is the branch of astrophysics that specializes in the study of the Sun. It deals with detailed measurements that are possible only for our closest star. It intersects with many disciplines of pure physics, astrophysics, and computer science, including fluid dynamics, plasma physics including magnetohydrodynamics, seismology, particle physics, atomic physics, nuclear physics, stellar evolution, space physics, spectroscopy, radiative transfer, applied optics, signal processing, computer vision, computational physics, stellar physics and solar astronomy.
Aníbal Domingo Fernández is an Argentine Justicialist Party politician, lawyer, and certified public accountant. Throughout his career, he has remained a close ally to the former Presidents Néstor Kirchner and Cristina Fernández de Kirchner. Since 2021, he has served as Argentina's Minister of Security, in the cabinet of President Alberto Fernández.
Heliophysics is the physics of the Sun and its connection with the Solar System. NASA defines heliophysics as "(1) the comprehensive new term for the science of the Sun - Solar System Connection, (2) the exploration, discovery, and understanding of Earth's space environment, and (3) the system science that unites all of the linked phenomena in the region of the cosmos influenced by a star like our Sun."
Joan Feynman was an American astrophysicist. She made contributions to the study of solar wind particles and fields, sun-Earth relations, and magnetospheric physics. In particular, Feynman was known for developing an understanding of the origin of auroras. She was also known for creating a model that predicts the number of high-energy particles likely to hit a spacecraft over its lifetime, and for uncovering a method for predicting sunspot cycles.
In solar physics, a coronal loop is a well-defined arch-like structure in the Sun's atmosphere made up of relatively dense plasma confined and isolated from the surrounding medium by magnetic flux tubes. Coronal loops begin and end at two footpoints on the photosphere and project into the transition region and lower corona. They typically form and dissipate over periods of seconds to days and may span anywhere from 1 to 1,000 megametres in length.
Helmet streamers, also known as coronal streamers, are elongated cusp-like structures in the Sun's corona which are often visible in white-light coronagraphs and during solar eclipses. They are closed magnetic loops which lie above divisions between regions of opposite magnetic polarity on the Sun's surface. The solar wind elongates these loops to pointed tips which can extend a solar radius or more into the corona.
Gloria Dubner is an Argentinian astrophysicist and Director of the Instituto de Astronomía y Física del Espacio in Buenos Aires and a Senior Researcher at the National Scientific and Technical Research Council. She is known for her research on supernovas.
Sarah E. Gibson is an American solar physicist. She is a Senior Scientist and past Director of the High Altitude Observatory in Boulder, Colorado. She is noted for extensive work developing the theory of coronal mass ejections (CMEs) and their precursors, and for organizing scientific collaborations that advance global understanding of the Sun and heliosphere. She is a recipient of the Solar Physics Division's Karen Harvey Prize for early achievement in solar physics, has been a member of the National Academy's Space Studies Board and co-chair of its Committee on Solar and Space Physics, and is Past President of the IAU's Division E. As of 2019, Dr. Gibson is the Project Scientist for the PUNCH Small Explorer mission being built for NASA.
Lidia van Driel-Gesztelyi is a Hungarian solar scientist and professor of physics at the Mullard Space Science Laboratory of University College London. She also maintains affiliations with Solar and Stellar Activity Research Team at Konkoly Observatory of the Hungarian Academy of Sciences and the Space Research Laboratory (LESIA) of Paris Observatory. She has been Editor-in-Chief of the journal Solar Physics since 2005 and has served in leadership roles within the International Astronomical Union.
Marta Graciela Rovira is an Argentine astrophysics researcher and was first woman to be named president of CONICET, the government agency that directs and coordinates most of the academic research performed in universities and institutes throughout the country.
Solar radio emission refers to radio waves that are naturally produced by the Sun, primarily from the lower and upper layers of the atmosphere called the chromosphere and corona, respectively. The Sun produces radio emissions through four known mechanisms, each of which operates primarily by converting the energy of moving electrons into radiation. The four emission mechanisms are thermal bremsstrahlung (free-free) emission, gyromagnetic emission, plasma emission, and electron-cyclotron maser emission. The first two are incoherent mechanisms, which means that they are the summation of radiation generated independently by many individual particles. These mechanisms are primarily responsible for the persistent "background" emissions that slowly vary as structures in the atmosphere evolve. The latter two processes are coherent mechanisms, which refers to special cases where radiation is efficiently produced at a particular set of frequencies. Coherent mechanisms can produce much larger brightness temperatures (intensities) and are primarily responsible for the intense spikes of radiation called solar radio bursts, which are byproducts of the same processes that lead to other forms of solar activity like solar flares and coronal mass ejections.
In solar physics, a transequatorial loop is a structure present in the solar corona that connects two different regions of opposite magnetic polarity in opposite hemispheres of the Sun. These connected regions are not limited to active regions, but are most commonly found during the times of maximum solar activity, the solar maximum.
Kelly Korreck is an American space scientist. She is currently an astrophysicist at the Center for Astrophysics | Harvard & Smithsonian and Program Scientist at NASA as head of operations for the Solar Wind Electrons Alphas and Protons (SWEAP) instrument aboard the Parker Solar Probe spacecraft.
Natchimuthuk Gopalswamy is an American solar physicist. He is currently a staff scientist at the Heliophysics Division of NASA’s Goddard Space Flight Center.
References
- ↑ Zhang, Sarah. "Argentina Has More Women in Science—But It Hasn't Fixed Sexism". Wired. ISSN 1059-1028 . Retrieved 2022-06-12.
- 1 2 3 "International Astronomical Union | IAU". www.iau.org. Retrieved 2022-06-11.
- ↑ "Tormentas solares: científicos explican cómo se detectan y qué se puede hacer para evitar sus consecuencias en la Tierra". LA NACION (in Spanish). 2022-02-22. Retrieved 2022-06-12.
- ↑ "C. H. Mandrini". scholar.google.com.ar. Retrieved 2022-06-12.
- ↑ "From the Sun to the terrestrial surface: understanding the chain". www.issibern.ch. Retrieved 2022-06-12.
- ↑ "The enduring mystery of the solar corona". Physics World. 2021-09-16. Retrieved 2022-06-12.
- ↑ "Cristina Mandrini was appointed president of the Steering Committee of the "Sun and Heliosphere" Division of the IAU" (in Spanish). Retrieved 2022-06-11.
- ↑ "Cristina Mandrini appointed president of the IAU Division E". www.springer.com. Retrieved 2022-06-11.
- ↑ "International Astronomical Union | IAU". www.iau.org. Retrieved 2022-06-11.
- ↑ "Mandrini, Cristina Hemilse". TWAS. Retrieved 2022-06-11.
- ↑ DF, Premio para profesores del. "Premios de la ANCEFN para Hernán Grecco y Cristina Mandrini". df.uba.ar. Retrieved 2022-06-11.
- ↑ www.e-dynamic.com.ar; dynamicIce. "- Tomo 70 - Año 2018". www.ancefn.org.ar. Retrieved 2022-06-11.
- ↑ "Solar Physics". Springer. Retrieved 2022-06-11.