- Space Exploration
One of the most perplexing problems in modern astrophysics, an observed shortage in the predicted number of neutrinos emanating from the Sun, appeared to be finally resolved during the year. Detailed theoretical studies of nuclear reactions in the Sun’s core had predicted that energy is released in the form of gamma rays, thermal energy, and neutrinos. The gamma rays and thermal energy slowly diffuse to the solar surface and are eventually observed as visible light and other electromagnetic radiation. Neutrinos are electrically neutral particles that travel almost unaffected through the Sun and interplanetary space on their way to Earth. Beginning in the late 1960s, scientists sought to detect these elusive particles directly. Because neutrinos interact so weakly with matter, detectors containing enormous quantities of mass were built to detect them. These were placed deep underground to allow neutrinos originating in the Sun to be distinguished from background galactic cosmic rays. Despite many experiments employing a variety of detectors, scientists consistently had observed only about a third of the predicted neutrino flux.
Neutrinos come in three varieties, or flavours—electron, muon, and tau. Because nuclear fusion in the Sun’s core should produce only electron neutrinos, most of the earlier experiments had been designed to detect only that flavour. The Sudbury Neutrino Observatory (SNO), sited deep inside a Canadian nickel mine, was built to have enhanced sensitivity to muon and tau neutrinos. It used as its detector a 1,000-ton sphere of extremely pure heavy water (water molecules in which the two hydrogen atoms are replaced with deuterium, one of hydrogen’s heavier isotopes). A second facility, called Super-Kamiokande and located in a zinc mine in Japan, employed a tank of 50,000 tons of ultrapure ordinary water to detect electron and muon neutrinos. In 2001 the international collaboration running SNO, headed by Art McDonald of Queen’s University at Kingston, Ont., reported evidence derived from SNO and Super-Kamiokande data for the detection of the missing two-thirds of the neutrino flux. The results confirmed the theory that electron neutrinos transform, or oscillate, among the three possible flavours on their journey to Earth. Oscillation also implied that neutrinos have a tiny but finite mass and thus make a contribution to the nonluminous, unobserved “dark matter” in the universe. (See Physics.)
The detection of planets orbiting other stars was first announced in 1995. By the beginning of 2001 about 50 extrasolar planets had been reported, and by year’s end the number had risen to more than 70. Most of the planets found to date are quite different from those in Earth’s solar system. Many are large (as much as 20 times the mass of Jupiter) and often move in elliptical orbits quite close to their parent stars.
During the year, for the first time, a planetary system remarkably similar to Earth’s solar system was detected. Geoffrey Marcy of the University of California, Berkeley, Paul Butler of the Carnegie Institution of Washington, D.C., and their collaborators reported that a star visible to the naked eye, 47 Ursae Majoris, is orbited by at least two planets. The presence of one planet had been known since 1996, but the new discovery changed astronomers’ picture of the system in important ways. One planet has a mass at least three-fourths that of Jupiter, and the other has at least two and a half times Jupiter’s mass. Interestingly, the ratio of their masses is close to the ratio of the masses of Saturn and Jupiter. Both extrasolar planets move in nearly circular orbits, a property that was thought to increase the odds that the system contains Earth-like planets as well.