Network analyzer (electrical)

For the majority of numbered asteroids, almost nothing is known apart from a few physical parameters. Hundreds of these (See Category:Asteroid stubs) have their own Wikipedia page, where the only information is their name and discovery circumstances plus a table of orbital elements and some physical characteristics often only estimated.

The aim of this page is to provide a reference explaining where the physical data for such generic asteroids comes from.

Due to the various ages of the single asteroid articles, the reference below may not be accurate for all asteroid articles.

Dimensions

Data from the IRAS minor planet survey or the Midcourse Space Experiment (MSX) minor planet survey (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 are tabulated in the PDS, 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.

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 $d=(abc{)}^{\frac{1}{3}}$ for consistency, and obtains the three diameters:

$a=d({\mu }^2\nu {)}^{\frac{1}{3}}$

$b=d{\left(\frac{\nu }{\mu }\right)}^{\frac{1}{3}}$

$c=\frac{d}{({\nu }^2\mu {)}^{\frac{1}{3}}}$

Mass

DTZ's public sale group in Singapore auctions all forms of residential, workplace and retail properties, outlets, homes, lodges, boarding homes, industrial buildings and development websites. Auctions are at present held as soon as a month.

We will not only get you a property at a rock-backside price but also in an space that you've got longed for. You simply must chill out back after giving us the accountability. We will assure you 100% satisfaction. Since we now have been working in the Singapore actual property market for a very long time, we know the place you may get the best property at the right price. You will also be extremely benefited by choosing us, as we may even let you know about the precise time to invest in the Singapore actual property market.

The Hexacube is offering new ec launch singapore business property for sale Singapore investors want to contemplate. Residents of the realm will likely appreciate that they'll customize the business area that they wish to purchase as properly. This venture represents one of the crucial expansive buildings offered in Singapore up to now. Many investors will possible want to try how they will customise the property that they do determine to buy by means of here. This location has offered folks the prospect that they should understand extra about how this course of can work as well.

Singapore has been beckoning to traders ever since the value of properties in Singapore started sky rocketing just a few years again. Many businesses have their places of work in Singapore and prefer to own their own workplace area within the country once they decide to have a everlasting office. Rentals in Singapore in the corporate sector can make sense for some time until a business has discovered a agency footing. Finding Commercial Property Singapore takes a variety of time and effort but might be very rewarding in the long term.

is changing into a rising pattern among Singaporeans as the standard of living is increasing over time and more Singaporeans have abundance of capital to invest on properties. Investing in the personal properties in Singapore I would like to applaud you for arising with such a book which covers the secrets and techniques and tips of among the profitable Singapore property buyers. I believe many novice investors will profit quite a bit from studying and making use of some of the tips shared by the gurus." – Woo Chee Hoe Special bonus for consumers of Secrets of Singapore Property Gurus Actually, I can't consider one other resource on the market that teaches you all the points above about Singapore property at such a low value. Can you? Condominium For Sale (D09) – Yong An Park For Lease

In 12 months 2013, c ommercial retails, shoebox residences and mass market properties continued to be the celebrities of the property market. Models are snapped up in report time and at document breaking prices. Builders are having fun with overwhelming demand and patrons need more. We feel that these segments of the property market are booming is a repercussion of the property cooling measures no.6 and no. 7. With additional buyer's stamp responsibility imposed on residential properties, buyers change their focus to commercial and industrial properties. I imagine every property purchasers need their property funding to understand in value. Barring detailed mass determinations, the mass M can be estimated from the diameter and (assumed) density values ρ worked out as below.

$M=\frac{\pi abc\rho }{6}$

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, or when the asteroid has an orbiting companion of known orbital radius. The masses of the largest asterois 1 Ceres, 2 Pallas, and 4 Vesta can also be obtained from perturbations of Mars. 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, one has to resort to enlightened guesswork. See Carry for a summary.

For many asteroids a value of ρ~2 g/cm³ 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/cm³. (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/cm³) is a better guess.

Surface gravity

Mining Engineer (Excluding Oil ) Truman from Alma, loves to spend time knotting, largest property developers in singapore developers in singapore and stamp collecting. Recently had a family visit to Urnes Stave Church.

Spherical body

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

$g_{\mathrm{s}\mathrm{p}\mathrm{h}\mathrm{e}\mathrm{r}\mathrm{i}\mathrm{c}\mathrm{a}\mathrm{l}}=\frac{GM}{r^2}$

Where G = 6.6742Template:E m³s⁻²kg⁻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 centripetall acceleration experienced at a latitude θ is

$g_{\mathrm{c}\mathrm{e}\mathrm{n}\mathrm{t}\mathrm{r}\mathrm{i}\mathrm{f}\mathrm{u}\mathrm{g}\mathrm{a}\mathrm{l}}=-{\left(\frac{2\pi }{T}\right)}^{2}r\sin \theta$

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

$g_{\mathrm{e}\mathrm{f}\mathrm{f}\mathrm{e}\mathrm{c}\mathrm{t}\mathrm{i}\mathrm{v}\mathrm{e}}=g_{\mathrm{g}\mathrm{r}\mathrm{a}\mathrm{v}\mathrm{i}\mathrm{t}\mathrm{a}\mathrm{t}\mathrm{i}\mathrm{o}\mathrm{n}\mathrm{a}\mathrm{l}}+g_{\mathrm{c}\mathrm{e}\mathrm{n}\mathrm{t}\mathrm{r}\mathrm{i}\mathrm{f}\mathrm{u}\mathrm{g}\mathrm{a}\mathrm{l}}.$

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:

$v_e=\sqrt{2gr}$

Rotation period

Rotation period is usually taken from lightcurve parameters at the PDS.

Spectral class

Spectral class is usually taken from the Tholen classification at the PDS.

Absolute magnitude

Absolute magnitude is usually given by the IRAS minor planet survey or the MSX minor planet survey (available at the PDS).

Albedo

Usually given by the IRAS minor planet survey or the MSX minor planet survey (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 then obtained by equating the mean incident and radiated heat power. The total incident power is:

$R_{\text{in}}=\frac{(1-A)L_0\pi r^2}{4\pi a^2},$

where $A$ is the asteroid albedo (precisely, the Bond albedo), $a$ its semi-major axis, $L_0$ is the solar luminosity (i.e. total power output 3.827×10²⁶ W), and $r$ the asteroid's radius. It has been assumed that: the absorptivity is $1-A$, 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:

$R_{\text{out}}=4\pi r^2ϵ\sigma T^4\frac{}{},$

where $\sigma$ is the Stefan-Boltzmann constant (5.6704×10⁻⁸ W/m²K⁴), $T$ is the temperature in kelvins, and $ϵ$ is the asteroid's infra-red emissivity. Equating $R_{\text{in}}=R_{\text{out}}$, one obtains

$T={\left(\frac{(1-A)L_0}{ϵ\sigma 16\pi a^2}\right)}^{1/4}$

The standard value of $ϵ$=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

$T_{ss}=\sqrt{2}T\approx 1.41T,$

where $T$ is the average temperature calculated as above.

At perihelion, the radiation is maximised, and

$T_{ss}^{\mathrm{m}\mathrm{a}\mathrm{x}}=\sqrt{\frac{2}{1-e}}T,$

where $e$ 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,

$T=\mathrm{c}\mathrm{o}\mathrm{n}\mathrm{s}\mathrm{t}\mathrm{a}\mathrm{n}\mathrm{t}\times \frac{1}{\sqrt{d}},$

where $d$ 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, 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. Up-to-date information on pole orientation of several dozen asteroids is provided by Doc. Mikko Kaasalainen, and can be used to determine axial tilt.

Another source of useful information is NASA's orbit calculator.

External links

• The Planetary Data System (PDS) Small Bodies Node