For the majority of numbered asteroids, almost nothing is known apart from a few physical parameters and orbital elements and some physical characteristics are often only estimated. The physical data is determined by making certain standard assumptions.

## Contents

## Dimensions

Data from the IRAS minor planet survey^{[1]}
or the Midcourse Space Experiment (MSX) minor planet survey^{[2]} (available at the Planetary Data System Small Bodies Node (PDS)) is the usual source of the diameter.

For many asteroids, lightcurve analysis provides estimates of pole direction and diameter ratios. Pre-1995 estimates collected by Per Magnusson^{[3]} are tabulated in the PDS,^{[4]} with the most reliable data being the *syntheses* labeled in the data tables as "Synth". More recent determinations for several dozens of asteroids are collected at the web page of a Finnish research group in Helsinki which is running a systematic campaign to determine poles and shape models from lightcurves.^{[5]}

These data can be used to obtain a better estimate of dimensions. A body's dimensions are usually given as a tri-axial ellipsoid, the axes of which are listed in decreasing order as *a*×*b*×*c*. If we have the diameter ratios *μ* = *a*/*b*, *ν* = *b*/*c* from lightcurves, and an IRAS mean diameter d, one sets the geometric mean of the diameters for consistency, and obtains the three diameters:

## Mass

Barring detailed mass determinations,^{[6]} the mass *M* can be estimated from the diameter and (assumed) density values *ρ* worked out as below.

Such estimates can be indicated as approximate by use of a tilde "~". Besides these "guesstimates", masses can be obtained for the larger asteroids by solving for the perturbations they cause in each other's orbits,^{[7]} or when the asteroid has an orbiting companion of known orbital radius. The masses of the largest asteroids 1 Ceres, 2 Pallas, and 4 Vesta can also be obtained from perturbations of Mars.^{[8]}
While these perturbations are tiny, they can be accurately measured from radar ranging data from the Earth to spacecraft on the surface of Mars, such as the Viking landers.

## Density

Apart from a few asteroids whose densities have been investigated,^{[6]} one has to resort to enlightened guesswork. See Carry^{[9]} for a summary.

For many asteroids a value of *ρ*~2 g/cm^{3} has been assumed.

However, density depends on the asteroid's spectral type. Krasinsky *et al.* gives calculations for the mean densities of C, S, and M class asteroids as 1.38, 2.71, and 5.32 g/cm^{3}.^{[10]} (Here "C" included Tholen classes C, D, P, T, B, G, and F, while "S" included Tholen classes S, K, Q, V, R, A, and E). Assuming these values (rather than the present ~2 g/cm^{3}) is a better guess.

## Surface gravity

### Spherical body

For a spherical body, the gravitational acceleration at the surface (*g*), is given by

Where *G* = 6.6742×10^{−11} m^{3}s^{−2}kg^{−1} is the gravitational constant, *M* is the mass of the body, and *r* its radius.

### Irregular body

For irregularly shaped bodies, the surface gravity will differ appreciably with location. The above formula then is only an approximation, as the calculations become more involved. The value of *g* at surface points closer to the center of mass is usually somewhat greater than at surface points farther out.

### Centripetal force

On a rotating body, the apparent weight experienced by an object on the surface is reduced by the centripetal force, when one is away from the poles. The centripetal acceleration experienced at a latitude θ is

where *T* is the rotation period in seconds, *r* is the equatorial radius, and θ is the latitude. Its magnitude is maximized when one is at the equator, and sinθ=1. The negative sign indicates that it acts in the opposite direction to the gravitational acceleration *g*.

The effective acceleration is

### Close binaries

If the body in question is a member of a close binary with components of comparable mass, the effect of the second body may also be non-negligible.

## Escape velocity

For surface gravity *g* and radius *r* of a spherically symmetric body, the escape velocity is:

## Rotation period

Rotation period is usually taken from lightcurve parameters at the PDS.^{[11]}

## Spectral class

Spectral class is usually taken from the Tholen classification at the PDS.^{[12]}

## Absolute magnitude

Absolute magnitude is usually given by the IRAS minor planet survey^{[1]} or the MSX minor planet survey^{[2]} (available at the PDS).

## Albedo

Astronomical albedos are usually given by the IRAS minor planet survey^{[1]} or the MSX minor planet survey^{[2]} (available at the PDS). These are *geometric albedos*. If there is no IRAS/MSX data a rough average of 0.1 can be used.

## Surface temperature

### Mean

The simplest method which gives sensible results is to assume the asteroid behaves as a greybody in equilibrium with the incident solar radiation. Then, its mean temperature is obtained by equating the mean incident and radiated heat power. The total incident power is:

where is the asteroid albedo (precisely, the Bond albedo), its semi-major axis, is the solar luminosity (i.e. total power output 3.827×10^{26} W), and the asteroid's radius. It has been assumed that: the absorptivity is , the asteroid is spherical, it is on a circular orbit, and that the Sun's energy output is isotropic.

Using a greybody version of the Stefan-Boltzmann law, the radiated power (from the entire spherical surface of the asteroid) is:

where is the Stefan-Boltzmann constant (5.6704×10^{−8} W/m²K^{4}), is the temperature in kelvins, and is the asteroid's infra-red emissivity. Equating , one obtains

The standard value of =0.9, estimated from detailed observations of a few of the large asteroids is used.

While this method gives a fairly good estimate of the average surface temperature, the local temperature varies greatly, as is typical for bodies without atmospheres.

### Maximum

A rough estimate of the maximum temperature can be obtained by assuming that when the Sun is overhead, the surface is in thermal equilibrium with the instantaneous solar radiation. This gives *average* "sub-solar" temperature of

where is the average temperature calculated as above.

At *perihelion*, the radiation is maximised, and

where is the eccentricity of the orbit.

### Temperature measurements and regular temperature variations

Infra-red observations are commonly combined with albedo to measure the temperature more directly. For example, L.F.Lim et al. [Icarus, Vo. 173, 385 (2005)] does this for 29 asteroids. However, it should be pointed out that these are measurements for *a particular observing day*, and that the asteroid's surface temperature will change in a regular way depending on its distance from the Sun. From the Stefan-Boltzmann calculation above,

where is the distance from the Sun on any particular day. If the day of the relevant observations is known, the distance from the Sun on that day can be obtained online from e.g. the NASA orbit calculator,^{[13]} and corresponding temperature estimates at perihelion, aphelion, etc. can be obtained from the expression above.

### Albedo inaccuracy problem

There is a snag when using these expressions to estimate the temperature of a particular asteroid. The calculation requires the Bond albedo *A* (the proportion of total incoming power reflected, taking into account all directions), while the IRAS and MSX albedo data that is available for asteroids gives only the geometric albedo *p* which characterises only the strength of light reflected back to the source (the Sun).

While these two albedos are correlated, the numerical factor between them depends in a very nontrivial way on the surface properties. Actual measurements of Bond albedo are not forthcoming for the majority of asteroids because they require measurements from high phase angles that can only be acquired by spacecraft that pass near or beyond the asteroid belt. Some complicated modelling of surface and thermal properties can lead to estimates of the Bond albedo given the geometric one, but this far is beyond the scope of a quick estimate for these articles. It can be obtained for some asteroids from scientific publications.

For want of a better alternative for most asteroids, the best that can be done here is to assume that these two albedos are equal, but keep in mind that there is an inherent inaccuracy in the resulting temperature values.

*How large is this inaccuracy?*

A glance at the examples in this table shows that for bodies in the asteroid albedo range, the typical difference between Bond and geometric albedo is 20% or less, with either quantity capable of being larger. Since the calculated temperature varies as (1-*A*)^{1/4}, the dependence is fairly weak for typical asteroid *A*≈*p* values of 0.05−0.3.

The typical inaccuracy in calculated temperature *from this source alone* is then found to be about 2%. This translates to an uncertainty of about ±5 K for maximum temperatures.

## Other common data

Some other information for large numbers of asteroids can be found at the Planetary Data System Small Bodies Node.^{[14]} Up-to-date information on pole orientation of several dozen asteroids is provided by Doc. Mikko Kaasalainen,^{[5]} and can be used to determine axial tilt.

Another source of useful information is NASA's orbit calculator.^{[13]}

## References

- ^
^{a}^{b}^{c}"IRAS Minor Planet Survey Supplemental IRAS Minor Planet Survey". PDS Asteroid/Dust Archive. Archived from the original on 2006-09-02. Retrieved 2006-10-21. - ^
^{a}^{b}^{c}"Midcourse Space Experiment (MSX) Infrared Minor Planet Survey". PDS Asteroid/Dust Archive. Archived from the original on 2006-09-02. Retrieved 2006-10-21. **^**Magnusson, Per (1989). "Pole determinations of asteroids". In Richard P. Binzel; Tom Gehrels; Mildred S. Matthews (eds.).*Asteroids II*. Tucson: University of Arizona Press. pp. 1180–1190.**^**"Asteroid Spin Vectors". Archived from the original on 2006-09-02. Retrieved 2006-10-21.- ^
^{a}^{b}Modeled asteroids.*rni.helsinki.fi*. 2006-06-18. - ^
^{a}^{b}For example "Asteroid Densities Compilation". PDS Asteroid/Dust Archive. Archived from the original on 2006-09-02. Retrieved 2006-10-21. **^**Hilton, James L. (November 30, 1999). "Masses of the Largest Asteroids". Archived from the original on February 12, 2009. Retrieved 2009-09-05.**^**Pitjeva, E. V. (2004).*Estimations of masses of the largest asteroids and the main asteroid belt from ranging to planets, Mars orbiters and landers*. 35th COSPAR Scientific Assembly. Held 18–25 July 2004. Paris, France. p. 2014. Bibcode:2004cosp...35.2014P.**^**Benoit Carry, Density of asteroids,*Planetary & Space Science*to be published (accessed Dec. 20, 2013**^**Krasinsky, G. A.; Pitjeva, E. V.; Vasilyev, M. V.; Yagudina, E. I. (July 2002). "Hidden Mass in the Asteroid Belt".*Icarus*.**158**(1): 98–105. Bibcode:2002Icar..158...98K. doi:10.1006/icar.2002.6837.**^**"Asteroid Lightcurve Parameters". PDS Asteroid/Dust Archive. Archived from the original on 2006-09-02. Retrieved 2006-10-21.**^**Asteroid Taxonomies*PDS Asteroid/Dust Archive*. 2006-10-21.- ^
^{a}^{b}"Orbit Diagrams". NASA. Retrieved 2006-06-18. **^**"Asteroid Data Sets". PDS Asteroid/Dust Archive. Archived from the original on 2006-09-28. Retrieved 2006-10-21.