Jupiter mass and diameter relationship

Planetary Science

jupiter mass and diameter relationship

Jul 18, Jupiter, Earth, Ratio (Jupiter/Earth). Mass ( kg), 1,, , Equatorial radius (1 bar level) (km), 71,, 6,, Jupiter has a diameter of about 88, miles (, kilometers) which is more than 11 times the diameter of Earth. It's volume is over 1, times the volume. diameter, vs Earth. Earth, mass. The densities (kg/m3) are somewhat similar, so mass follows volume. Remembering the size of Earth, and the 1: 10 : size relation, you then know the size of Jupiter and the Sun, too. And area and.

The orbits of the inner planets of the Solar System, with Jupiter and the donut-shaped asteroid belt is located between them. Wikipedia Commons The Earth has an orbital period of This means that every four years in what is known as a Leap Yearthe Earth calendar must include an extra day. Though technically a full day is considered to be 24 hours long, our planet takes precisely 23h 56m and 4 s to complete a single sidereal rotation 0. But combined with its orbital period around the Sun, the time between one sunrise and another a Solar Day is 24 hours.

Viewed from the celestial north pole, the motion of Earth and its axial rotation appear counterclockwise. From the vantage point above the north poles of both the Sun and Earth, Earth orbits the Sun in a counterclockwise direction.

In addition to producing variations in temperature, this also results in variations in the amount of sunlight a hemisphere receives during the course of a year. Meanwhile, Jupiter orbits the Sun at an average distance semi-major axis of , km 5.

jupiter mass and diameter relationship

At this distance, Jupiter takes In other words, a single Jovian year lasts the equivalent of 4, Therefore, a single Jovian year lasts 10, As a rule, air pressure and density decrease the higher one goes into the atmosphere and the farther one is from the surface. However, the relationship between temperature and altitude is more complicated, and may even rise with altitude in some cases. The one exception is the Thermoposphere, where the phenomena known as Aurora Borealis and Aurara Australis aka.

MASS-RADIUS RELATIONSHIPS FOR EXOPLANETS

The Northern and Southern Lights are known to take place. Much like Earth, Jupiter experiences auroras near its northern and southern poles. But on Jupiter, the auroral activity is much more intense and rarely ever stops. Jupiter also experiences violent weather patterns. For our present purposes, it is most useful to compare EOS for different compositions of matter constructed according to consistent prescriptions. The use of wide-ranging EOS constructed using optimized algorithms, and wide-ranging sets of electronic structure calculations made using a consistent method that reproduces TFD at extreme compressions, allows us to avoid any reliance on extrapolating using ad hoc functional forms such as Vinet and Birch—Murnaghan for pressure—density relations, which can give unquantified uncertainties outside the range of the fitting data.

Dynamic Loading Experiments The canonical experimental technique for studying the properties at matter at high pressure is shock loading, using a variety of methods to induce a shock wave. Shock measurements of EOS are often performed relative to a reference material, but an attraction of shock loading is that experiments can in principle be configured to yield absolute measurements, if the shock is induced by the impact of a projectile with a target of the same material.

Indeed, the pressure standards in static compression apparatus such as diamond anvil cells are ultimately calibrated against absolute shock measurements.

Jupiter mass - Wikipedia

Although the timescale in dynamic loading experiments is typically nanoseconds to microseconds, typical equilibration times for electrons and atomic vibrations are much shorter, so inferred states used for testing and calibrating EOS are in thermodynamic equilibrium and thus equivalent to quasistatic compression measurements made in presses such as diamond anvil cells. Indeed, the difference in timescale between dynamic and quasistatic loading is less than the difference between the latter and planetary ages.

Although EOS measurements are in thermodynamic equilibrium with respect to a given phase of matter, the time dependence of phase transitions must be considered: The effects of time dependence are also evident as hysteresis in the location of the phase change on loading compared with unloading. In shock loading, the entropy increases with compression, so the temperature rises faster with compression than it does along an isentrope.

Jupiter Compared to Earth - Universe Today

While a direct measurement of a relevant state is preferable, shock-derived EOS are likely to be adequate for exoplanets over a wide range of pressures. Furthermore, if a theoretical EOS is validated by shock experiments, this provides reasonable confidence that the EOS is valid at lower temperatures.

A more serious limitation with shock experiments is that, for a given material and starting state, there is a limit to the compression that can be achieved by the passage of a single shock, and therefore a limit to the range of compressions that can be deduced along isentropes. However, this compression discussed further below for different compositions of matter is adequate to explore matter into the massive exoplanet regime.

The compression limit can be circumvented through the use of multiple shocks, which induce lower temperatures than a single shock to the same pressure.

The ultimate limit for an infinite sequence of infinitesimal shocks is a ramp compression. Experimental techniques have thus been available to develop and test EOS under conditions relevant to exoplanets, and planned developments should provide the first direct measurements of matter under exoplanet core conditions. Spherical structures are certainly an adequate starting place for studies of exoplanets. The condition for isostatic equilibrium is that the stress induced by pressure variations is balanced by the gravitational acceleration g r: For Newtonian gravitation, by Gauss' theorem, g r can be expressed in terms of the mass enclosed within a given radius m r: In this way, the mass—radius condition is obtained in terms of pc as an independent parameter: In this case, the isostatic structure may be found more conveniently by starting with the desired masses of each component and solving the system of equations as an elliptic problem.

The radial variation was represented discretely by values at a finite series of radii. A series of solutions describing a mass—radius relation can be found efficiently by working upward in mass, and increasing the density at each radius by a constant factor, then calculating the modified equilibrium structure. We verified that this method of solution gave the same result as integration from the center to the surface, by comparison with structures comprising pure Fe.

In the present study, we usually chose an isentrope passing through a reasonable surface state, such as standard temperature and pressure STP for rock or metal, or a few atmospheres pressure and cryogenic temperatures for compositions that are gaseous at STP.

Isentropes were calculated by numerical integration of the relation using a procedure valid for EOS of arbitrary form Swift Mass—radius relations were calculated for a series of compositions of matter relevant to exo planets, using as a baseline EOS developed from and for shock wave applications, in particular the SESAME library Holianfor which the constituent assumptions and calibrations are reasonably well documented.

In degrees this is Notice that you need to convert arc seconds to degrees to use the angular size formula. Little Pluto is so small and far away that its angular diameter is very hard to measure. Only a large telescope above the Earth atmosphere like the Hubble Space Telescope can resolve its tiny disk. However, the discovery in of a moon, called Charon, orbiting Pluto gave another way to measure Pluto's diameter.

Every years, the orientation of Charon's orbit as seen from the Earth is almost edge-on, so you can see it pass in front of Pluto and then behind Pluto. This favorable orientation lasts about 5 years and, fortunately for us, it occurred from to When Pluto and Charon pass in front of each other, the total light from the Pluto-Charon system decreases.

The length of time it takes for the eclipse to happen and the speed that Charon orbits Pluto can be used to calculate their linear diameters. This eclipsing technique is also used to find the diameters of the very far away stars in a later chapter.

Another way to specify a planet's size is to use how much space it occupies, i.

jupiter mass and diameter relationship

Volume is important because it and the planet's composition determine how much heat energy a planet retains after its formation billions of years ago. Also, in order to find the important characteristic of density see the next sectionyou must know the planet's volume. Planets are nearly perfect spheres. Gravity compresses the planets to the most compact shape possible, a sphere, but the rapidly-spinning ones bulge slightly at the equator.

Jupiter Compared to Earth

This is because the inertia of a planet's material moves it away from the planet's rotation axis and this effect is strongest at the equator where the rotation is fastest Jupiter and Saturn have easily noticeable equatorial bulges. Notice that the diameter is cubed. Densities and Compositions An important property of a planet that tells what a planet is made of is its density. A planet's density is how much material it has in the space the planet occupies: Planets can have a wide range of sizes and masses but planets made of the same material will have the same density regardless of their size and mass.

For example, a huge, massive planet can have the same density as a small, low-mass planet if they are made of the same material. I will specify the density relative to the density of pure water because it has an easy density to rememeber: The four planets closest to the Sun Mercury, Venus, Earth, Mars are called the terrestrial planets because they are like the Earth: From top left and proceeding clockwise: Earth, Venus, Mercury, Mars at bottom left.

Since terrestrial planets have average densities greater than that for the silicate rocks on their surface, they must have denser material under the surface to make the overall average density what it is.

Iron and nickel are present in meteorites chunks of rock left over from the formation of the solar system and the presence of magnetic fields in some of the terrestrial planets shows that they have cores of iron and nickel.

Star Size Comparison 2

Magnetic fields can be produced by the motion of liquid iron and nickel. Putting these facts together leads to the conclusion that the terrestrial planets are made of silicate rock surrounding a iron-nickel core. The four giant planets beyond Mars Jupiter, Saturn, Uranus, Neptune are called the jovian planets because they are like Jupiter:

jupiter mass and diameter relationship