Raymond Jeanloz is a professor of Earth and planetary science (EPS) and Astronomy at the University of California, Berkeley. [1] Educated at the California Institute of Technology, Amherst College and at Deep Springs College, [2] his research contributions have been fundamental to understanding of the composition of the Earth and the behavior of materials under high temperatures and pressures. [3] Jeanloz has created tools and experiments that enable him to recreate and study deep interior conditions in a laboratory setting, [4] He is working with colleagues to investigate the conditions inside supergiant exoplanets. [5]
Jeanloz has chaired the National Research Council Board on Earth Sciences and Resources. [6] He is a co-editor of the Annual Review of Earth and Planetary Sciences [7] and serves on the Board of Directors of Annual Reviews. [8]
Jeanloz is also active in connecting science and policy in areas including international policy, resources and the environment, and science education. [4] [9] He has been particularly prominent in informing national and international security and nuclear weapons policy, [9] chairing the Committee on International Security and Arms Control at the National Academy of Sciences. [10] In 2009 he received the Leo Szilard Lectureship Award from the American Physical Society for "contributions to development of sound public policy for nuclear weapons management and nuclear non-proliferation." [3] Jeanloz became an Annenberg Distinguished Visiting Fellow at Stanford University's Hoover Institution in 2012. [11]
Raymond Jeanloz is one of four children of Roger W. Jeanloz, a professor in biological chemistry and molecular pharmacology at Harvard Medical School, and his wife Dorothea. [12] Raymond Jeanloz grew up in Massachusetts and spent two years at Deep Springs College, located in the Deep Springs Valley [2] between the White Mountains and Inyo Mountains in California. [13] His initial interests were in comparative literature and music. While he had some early exposure to geology, his interest in that field developed late in his undergraduate program. [14] Having also tried Hampshire College [4] [15] and taken a "gap period" of several months, Jeanloz completed his B.A. in geology at Amherst College in Massachusetts in 1975. [16] [14]
Jeanloz applied to the California Institute of Technology (Caltech) in part because of the Caltech Seismological Laboratory. His thesis advisor at Caltech was Thomas J. Ahrens. Jeanloz credits Ahrens and others for their mentorship and support, in helping him to learn about areas where he lacked scientific background and in encouraging him to explore new areas of research. [14] In 1979, Jeanloz received his Ph.D. from Caltech [16] for the thesis Physics of mantle and core minerals (1979). [17]
Jeanloz joined the faculty at Harvard University in 1979, [4] working at the intersection of materials science and physics. [14] He taught there until 1981. [4] In 1982, [18] he moved to the University of California, Berkeley where he became a professor of Earth and planetary science and of Astronomy. [19]
Jeanloz is a member of the National Academy of Sciences. He advises the US Government, the University of California and its national laboratories on a wide variety of issues including national security. He has chaired the Committee on International Security and Arms Control, and has been recognized by the Federation of American Scientists and the American Physical Society for shaping government policy. [4] [10] [3]
Jeanloz was an early researcher in mineral physics, and was one of those who proposed the field for recognition by the American Geophysical Union (AGU). [20] His work has connected mineral physics, chemistry, and materials science. [4] [16]
Nowadays, when people ask me, "What should I do?" I say, "Consider at least one possibility is to create a new field." – Raymond Jeanloz [14]
Jeanloz studies processes that occur under high temperatures and pressures, conditions that are characteristic of the interiors of planets and the core-mantle boundary of the Earth. [21] [22] [14] [15] Jeanloz studies planetary interiors and the properties of materials at high pressures to characterize the processes by which planets evolve over geological time periods. [23] [24] [14] [15] In the interiors of planets, pressure on materials can be millions of times higher than those at the Earth’s surface and materials can behave in very different ways. [4] Jeanloz has examined the properties and state equations of materials including alkali halides, alkaline-earth monoxides, silicate perovskite and iron. [15]
Jeanloz has created tools and experiments that enable him to recreate and study deep interior conditions in a laboratory setting, often by generating extremely high pressure in tiny amounts. [4] [24] He and his students have created new materials that can only be synthesized at extreme pressures, including ultra-hard diamond-like substances. [16] He has used diamond tips to simulate compression, creating diamond anvil cells capable of producing 4 to 5 million atmospheres, comparable to the pressures found at the center of the Earth. [25] He has created impact waves by shooting projectiles at high speeds, and generated high-energy laser pulses. [4] [24] He has furthered the use of techniques for shock-loading, deformation, spectroscopy, and phase equilibria. [15] By combining dynamic laser-induced shock waves and static diamond anvils, Jeanloz has found ways to study the behavior of materials at pressures that could range from millions to billions of atmospheres. This allows scientists to simulate conditions within giant and supergiant planets. [25] [26]
His research has led to greater understanding of how planets form, the composition of their interiors, and how those interiors behave. [4] [27] His research group is best known for experiments documenting that bridgmanite, [28] a high-pressure form of (Mg,Fe)SiO3, is the primary material making up Earth’s interior. [16] [25] He and his colleagues provided the first experimental determination of the temperature at Earth’s center, concluding that it is as hot as the Sun’s surface. [16] They also found evidence for chemical reactions between the rocky mantle and metallic core, likely making the core-mantle boundary one of Earth’s most dynamic regions. [16] [21] [22]
Jeanloz' group and their collaborators have modeled processes of diamond formation, indicating that diamonds may be hailing inside “icy” giant planets like Neptune. [29] They have helped characterize the primary constituents of giant planets and stars, the high-pressure fluid-metal forms of hydrogen and helium. They have determined that helium and hydrogen can form a metallic liquid alloy at the extreme pressures that occur at the cores of Jupiter and Saturn. [23] [30] [31] They have studied pressurized hydrogen and documented an insulator-to-metal transition in fluid hydrogen, identifying the conditions under which it turns into a metal. [32] [33] Their research also suggests that helium separates out of fluid metallic hydrogen inside Jupiter and Saturn, creating an immiscibility region in Jupiter and a four-layered planetary structure. [34]
In another collaboration Jeanloz has studied the behavior of a novel superionic form of water ice, one that is simultaneously liquid and solid and can conduct electricity as if it was a metal. The mantles of ice giant planets like Uranus and Neptune may contain superionic ice, possibly explaining some odd behaviors of their magnetic fields. [35] [36] His group’s experiments have also pioneered the discovery of crystal instabilities causing strain-induced amorphization and fracture-like processes, leading to new insights on how materials break. [37] [38]
A giant planet, sometimes referred to as a jovian planet, is a diverse type of planet much larger than Earth. Giant planets are usually primarily composed of low-boiling point materials (volatiles), rather than rock or other solid matter, but massive solid planets can also exist. There are four such planets in the Solar System: Jupiter, Saturn, Uranus, and Neptune. Many extrasolar giant planets have been identified.
In science and engineering the study of high pressure examines its effects on materials and the design and construction of devices, such as a diamond anvil cell, which can create high pressure. High pressure usually means pressures of thousands (kilobars) or millions (megabars) of times atmospheric pressure.
Earth's outer core is a fluid layer about 2,260 km (1,400 mi) thick, composed of mostly iron and nickel that lies above Earth's solid inner core and below its mantle. The outer core begins approximately 2,889 km (1,795 mi) beneath Earth's surface at the core-mantle boundary and ends 5,150 km (3,200 mi) beneath Earth's surface at the inner core boundary.
In planetary science, planetary differentiation is the process by which the chemical elements of a planetary body accumulate in different areas of that body, due to their physical or chemical behavior. The process of planetary differentiation is mediated by partial melting with heat from radioactive isotope decay and planetary accretion. Planetary differentiation has occurred on planets, dwarf planets, the asteroid 4 Vesta, and natural satellites.
The abundance of the chemical elements is a measure of the occurrences of the chemical elements relative to all other elements in a given environment. Abundance is measured in one of three ways: by mass fraction, by mole fraction, or by volume fraction. Volume fraction is a common abundance measure in mixed gases such as planetary atmospheres, and is similar in value to molecular mole fraction for gas mixtures at relatively low densities and pressures, and ideal gas mixtures. Most abundance values in this article are given as mass fractions.
A planetary core consists of the innermost layers of a planet. Cores may be entirely liquid, or a mixture of solid and liquid layers as is the case in the Earth. In the Solar System, core sizes range from about 20% to 85% of a planet's radius (Mercury).
The internal structure of Earth are the layers of the Earth, excluding its atmosphere and hydrosphere. The structure consists of an outer silicate solid crust, a highly viscous asthenosphere, and solid mantle, a liquid outer core whose flow generates the Earth's magnetic field, and a solid inner core.
George Wetherill was a physicist and geologist and the director emeritus of the department of terrestrial magnetism at the Carnegie Institution of Washington, DC, US.
An ice giant is a giant planet composed mainly of elements heavier than hydrogen and helium, such as oxygen, carbon, nitrogen, and sulfur. There are two ice giants in the Solar System: Uranus and Neptune.
The origin of water on Earth is the subject of a body of research in the fields of planetary science, astronomy, and astrobiology. Earth is unique among the rocky planets in the Solar System in having oceans of liquid water on its surface. Liquid water, which is necessary for all known forms of life, continues to exist on the surface of Earth because the planet is at a far enough distance from the Sun that it does not lose its water, but not so far that low temperatures cause all water on the planet to freeze.
Ho-Kwang (Dave) Mao is a Chinese-American geologist. He is the director of the Center for High Pressure Science and Technology Advanced Research in Shanghai, China. He was a staff scientist at Geophysical Laboratory of the Carnegie Institution for Science for more than 30 years. Mao is a recognized leading scientist in high pressure geosciences and physical science. There are two minerals named after him, Davemaoite and Maohokite.
Annual Review of Earth and Planetary Sciences is an annual peer-reviewed scientific journal published by Annual Reviews, which broadly covers Earth and planetary sciences, including geology, atmospheric sciences, climate, geophysics, environmental science, geological hazards, geodynamics, planet formation, and solar system origins. The co-editors are Katherine H. Freeman and Raymond Jeanloz. As of 2024, Journal Citation Reports gives the journal a 2023 impact factor of 11.3. As of 2023, it is being published as open access, under the Subscribe to Open model.
The history of scientific thought about the formation and evolution of the Solar System began with the Copernican Revolution. The first recorded use of the term "Solar System" dates from 1704. Since the seventeenth century, philosophers and scientists have been forming hypotheses concerning the origins of the Solar System and the Moon and attempting to predict how the Solar System would change in the future. René Descartes was the first to hypothesize on the beginning of the Solar System; however, more scientists joined the discussion in the eighteenth century, forming the groundwork for later hypotheses on the topic. Later, particularly in the twentieth century, a variety of hypotheses began to build up, including the now–commonly accepted nebular hypothesis.
The biological and geological future of Earth can be extrapolated based on the estimated effects of several long-term influences. These include the chemistry at Earth's surface, the cooling rate of the planet's interior, the gravitational interactions with other objects in the Solar System, and a steady increase in the Sun's luminosity. An uncertain factor is the pervasive influence of technology introduced by humans, such as climate engineering, which could cause significant changes to the planet. For example, the current Holocene extinction is being caused by technology, and the effects may last for up to five million years. In turn, technology may result in the extinction of humanity, leaving the planet to gradually return to a slower evolutionary pace resulting solely from long-term natural processes.
A gas giant is a giant planet composed mainly of hydrogen and helium. Jupiter and Saturn are the gas giants of the Solar System. The term "gas giant" was originally synonymous with "giant planet". However, in the 1990s, it became known that Uranus and Neptune are really a distinct class of giant planets, being composed mainly of heavier volatile substances. For this reason, Uranus and Neptune are now often classified in the separate category of ice giants.
Although diamonds on Earth are rare, extraterrestrial diamonds are very common. Diamonds so small that they contain only about 2000 carbon atoms are abundant in meteorites, and some of them formed in stars before the Solar System existed. High pressure experiments suggest large amounts of diamonds are formed from methane on the ice giant planets Uranus and Neptune, while some planets in other planetary systems may be almost pure diamond. Diamonds are also found in stars and may have been the first mineral ever to have formed.
The geochemistry of carbon is the study of the transformations involving the element carbon within the systems of the Earth. To a large extent this study is organic geochemistry, but it also includes the very important carbon dioxide. Carbon is transformed by life, and moves between the major phases of the Earth, including the water bodies, atmosphere, and the rocky parts. Carbon is important in the formation of organic mineral deposits, such as coal, petroleum or natural gas. Most carbon is cycled through the atmosphere into living organisms and then respirated back into the atmosphere. However an important part of the carbon cycle involves the trapping of living matter into sediments. The carbon then becomes part of a sedimentary rock when lithification happens. Human technology or natural processes such as weathering, or underground life or water can return the carbon from sedimentary rocks to the atmosphere. From that point it can be transformed in the rock cycle into metamorphic rocks, or melted into igneous rocks. Carbon can return to the surface of the Earth by volcanoes or via uplift in tectonic processes. Carbon is returned to the atmosphere via volcanic gases. Carbon undergoes transformation in the mantle under pressure to diamond and other minerals, and also exists in the Earth's outer core in solution with iron, and may also be present in the inner core.
The deep water cycle, or geologic water cycle, involves exchange of water with the mantle, with water carried down by subducting oceanic plates and returning through volcanic activity, distinct from the water cycle process that occurs above and on the surface of Earth. Some of the water makes it all the way to the lower mantle and may even reach the outer core. Mineral physics experiments show that hydrous minerals can carry water deep into the mantle in colder slabs and even "nominally anhydrous minerals" can store several oceans' worth of water.
Inner core super-rotation is the eastward rotation of the inner core of Earth relative to its mantle, for a net rotation rate that is usually faster than Earth as a whole. A 1995 model of Earth's dynamo predicted super-rotations of up to 3 degrees per year; the following year, this prediction was supported by observed discrepancies in the time that p-waves take to travel through the inner and outer core.
Over the years, our ability to detect, confirm, and characterize exoplanets and their atmospheres has improved, allowing researchers to begin constraining exoplanet interior composition and structure. While most exoplanet science is focused on exoplanetary atmospheric environments, the mass and radius of a planet can tell us about a planet's density, and hence, its internal processes. The internal processes of a planet are partly responsible for its atmosphere, and so they are also a determining factor in a planet's capacity to support life.
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