Magnetic reconnection shows the reconfiguration of magnetic field geometry. It plays an elemental role in the rapid release of magnetic energy and its conversion to other forms of energy in magnetized plasma systems throughout the universe.

Researchers led by Dr. Li Leping from National Astronomical Observatories of Chinese Academy of Sciences (NAOC) analyzed the evolution of magnetic reconnection and its nearby filament.

The solar wind is a flow of particles that comes off the sun at about one million miles per hour and travels throughout the entire solar system. First proposed in the 1950s by University of Chicago physicist Eugene Parker, the solar wind is visible in the halo around the sun during an eclipse and sometimes when the particles hit the Earth's atmosphere—as the aurora borealis, or northern lights.

While the solar wind protects Earth from other harmful particles coming from space, storms can also threaten our satellite and communications networks.

What is the solar wind?

The surface of the sun is blisteringly hot at 6,000 degrees Fahrenheit—but its atmosphere, called the corona, is more than a thousand times hotter. It is also incredibly active; those flares and loops are the halo you see around the sun when there's an eclipse.

The corona is so hot that the sun's gravity can't hold it, so particles are flung off into space and travel throughout the solar system in every direction. As the sun spins, burns and burps, it creates complex swirls and eddies of particles. These particles, mostly protons and electrons, are traveling about a million miles per hour as they pass Earth.

An orange pouch and a yellow cable are paving the way for missions to the moon. By monitoring space radiation and enabling faster communications, the Dosis-3D experiment and the Columbus Ka-band or ColKa terminal, respectively, are providing the insights needed to enable safer missions father out in space.

Orange Dosis-3D pouches are everywhere in the Columbus laboratory on the International Space Station. A series of active and passive dosimeters, they measure space radiation inside the module as well as how it penetrates the Space Station's walls.

Radiation levels in space are up to 15 times higher than on Earth. As soon as humans leave the protective shield that is Earth's atmosphere, space radiation becomes a serious concern.

The Columbus module is monitored by 11 passive dosimeters. The dosimeters are about the size of a pack of playing cards and attach to the walls of Columbus with Velcro. The detectors record how much radiation has been absorbed in total during the period they are in space.

This experiment has been monitoring radiation levels for a number of years and after each six-month crew rotation, the detectors are replaced to record changes in radiation.

The weathering of silicate rocks plays an important role to keep the climate on Earth clement. Scientists led by the University of Bern and the Swiss national center of competence in research (NCCR) PlanetS, investigated the general principles of this process. Their results could influence how we interpret the signals from distant worlds—including such that may hint towards life.

The conditions on Earth are ideal for life. Most places on our planet are neither too hot nor too cold and offer liquid water. These and other requirements for life, however, delicately depend on the right composition of the atmosphere.