File:Eunomia family.png
Summary
Diagrams showing the location and characteristics of the <a href="https://en.wikipedia.org/wiki/Eunomia_family" class="extiw" title="en:Eunomia family">Eunomia family</a> of <a href="https://en.wikipedia.org/wiki/asteroid" class="extiw" title="en:asteroid">asteroids</a>. Where circles are plotted, their diameter is proportional to the mean diameter of the asteroid.
In the top diagrams, the <a href="https://en.wikipedia.org/wiki/proper_orbital_elements" class="extiw" title="en:proper orbital elements">proper orbital elements</a> are plotted (<a href="https://en.wikipedia.org/wiki/inclination" class="extiw" title="en:inclination">inclination</a> ip vs. <a href="https://en.wikipedia.org/wiki/semi-major_axis" class="extiw" title="en:semi-major axis">semi-major axis</a> ap on the left, and <a href="https://en.wikipedia.org/wiki/inclination" class="extiw" title="en:inclination">inclination</a> ip vs. <a href="https://en.wikipedia.org/wiki/eccentricity_(orbit)" class="extiw" title="en:eccentricity (orbit)">eccentricity</a> ep on the right) for numbered <a href="https://en.wikipedia.org/wiki/asteroid" class="extiw" title="en:asteroid">asteroids</a> in the <a href="https://en.wikipedia.org/wiki/main_belt" class="extiw" title="en:main belt">main belt</a>.
In the bottom enlargements, one has:
- core family members (shown in red) are those identified by the 1995 Zappala (V. Zappala et al, Icarus Vol. 116, p. 291 (1995)) HCM method analysis. The data set <a rel="nofollow" class="external text" href="http://www.psi.edu/pds/archive/astdata/FAMILY/family.tab">is here</a>.
- interlopers (shown in green) were identified either:
- by the spectroscopic analysis of Lazzaro et al (Lazarro et al The Eunomia Family: A Visible Spectroscopic Survey, Icarus, Vol. 142, p. 445 (1999),
- and also by inspection of the <a rel="nofollow" class="external text" href="http://www.psi.edu/pds/archive/tax.html">PDS asteroid taxonomy data set</a> for non S-type members of the above Zappala 1995 data-set.
- numbered asteroids in general (shown as small blue dots), from the AstDys database.
The location of asteroids that are very large and/or explicitly named on the plot is shown by a light cross within the circle.
Asteroid diameters were obtained from two sources:
- (thick circles): From the IRAS survey, when available (data set <a rel="nofollow" class="external text" href="http://www.psi.edu/pds/archive/simps.html">here</a>).
- (thin circles): Otherwise, by assuming an albedo of 0.209 (same as <a href="https://en.wikipedia.org/wiki/15_Eunomia" class="extiw" title="en:15 Eunomia">15 Eunomia</a>), and estimating from absolute magnitudes from the AstOrb database <a rel="nofollow" class="external text" href="http://www.lowell.edu/users/elgb/">here</a>.
The diagrams were created by <a href="https://en.wikipedia.org/wiki/User:Deuar" class="extiw" title="en:User:Deuar">me</a> (Piotr Deuar) using proper element data for 96944 <a href="https://en.wikipedia.org/wiki/minor_planet" class="extiw" title="en:minor planet">minor planets</a>, which was obtained from the <a rel="nofollow" class="external text" href="http://hamilton.dm.unipi.it/cgi-bin/astdys/astibo?proper_elements:0;main">AstDys site</a>. Data was dated March 2005, calculation was by Z. Knezevic and A. Milani.
The top left plot is a slightly modified reduced version of <a href="https://en.wikipedia.org/wiki/Image:Asteroid_proper_elements_i_vs_a.png" class="extiw" title="en:Image:Asteroid proper elements i vs a.png">:Image:Asteroid_proper_elements_i_vs_a.png</a>.
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| Date/Time | Thumbnail | Dimensions | User | Comment | |
|---|---|---|---|---|---|
| current | 21:49, 16 January 2017 | | 1,200 × 990 (456 KB) | 127.0.0.1 (talk) | Diagrams showing the location and characteristics of the <a href="https://en.wikipedia.org/wiki/Eunomia_family" class="extiw" title="en:Eunomia family">Eunomia family</a> of <a href="https://en.wikipedia.org/wiki/asteroid" class="extiw" title="en:asteroid">asteroids</a>. Where circles are plotted, their diameter is proportional to the mean diameter of the asteroid. <p>In the <b>top diagrams</b>, the <a href="https://en.wikipedia.org/wiki/proper_orbital_elements" class="extiw" title="en:proper orbital elements">proper orbital elements</a> are plotted (<a href="https://en.wikipedia.org/wiki/inclination" class="extiw" title="en:inclination">inclination</a> <i>i<sub>p</sub></i> vs. <a href="https://en.wikipedia.org/wiki/semi-major_axis" class="extiw" title="en:semi-major axis">semi-major axis</a> <i>a<sub>p</sub></i> on the left, and <a href="https://en.wikipedia.org/wiki/inclination" class="extiw" title="en:inclination">inclination</a> <i>i<sub>p</sub></i> vs. <a href="https://en.wikipedia.org/wiki/eccentricity_(orbit)" class="extiw" title="en:eccentricity (orbit)">eccentricity</a> <i>e<sub>p</sub></i> on the right) for numbered <a href="https://en.wikipedia.org/wiki/asteroid" class="extiw" title="en:asteroid">asteroids</a> in the <a href="https://en.wikipedia.org/wiki/main_belt" class="extiw" title="en:main belt">main belt</a>. </p> <p>In the <b>bottom enlargements</b>, one has: </p> <ul> <li> <i>core</i> family members (shown in red) are those identified by the 1995 Zappala (V. Zappala et al, Icarus Vol. 116, p. 291 (1995)) HCM method analysis. The data set <a rel="nofollow" class="external text" href="http://www.psi.edu/pds/archive/astdata/FAMILY/family.tab">is here</a>.</li> <li> <i>interlopers</i> (shown in green) were identified either: <ul> <li> by the spectroscopic analysis of Lazzaro et al (Lazarro et al <i>The Eunomia Family: A Visible Spectroscopic Survey</i>, Icarus, Vol. 142, p. 445 (1999),</li> <li> and also by inspection of the <a rel="nofollow" class="external text" href="http://www.psi.edu/pds/archive/tax.html">PDS asteroid taxonomy data set</a> for non S-type members of the above Zappala 1995 data-set.</li> </ul> </li> <li> <i>numbered</i> asteroids in general (shown as small blue dots), from the AstDys database.</li> </ul> <p>The location of asteroids that are very large and/or explicitly named on the plot is shown by a light cross within the circle. </p> <p>Asteroid diameters were obtained from two sources: </p> <ul> <li> (<i>thick</i> circles): From the IRAS survey, when available (data set <a rel="nofollow" class="external text" href="http://www.psi.edu/pds/archive/simps.html">here</a>). </li> <li> (<i>thin</i> circles): Otherwise, by assuming an albedo of <b>0.209</b> (same as <a href="https://en.wikipedia.org/wiki/15_Eunomia" class="extiw" title="en:15 Eunomia">15 Eunomia</a>), and estimating from absolute magnitudes from the AstOrb database <a rel="nofollow" class="external text" href="http://www.lowell.edu/users/elgb/">here</a>. </li> </ul> <p>The diagrams were created by <a href="https://en.wikipedia.org/wiki/User:Deuar" class="extiw" title="en:User:Deuar">me</a> (Piotr Deuar) using proper element data for 96944 <a href="https://en.wikipedia.org/wiki/minor_planet" class="extiw" title="en:minor planet">minor planets</a>, which was obtained from the <a rel="nofollow" class="external text" href="http://hamilton.dm.unipi.it/cgi-bin/astdys/astibo?proper_elements:0;main">AstDys site</a>. Data was dated March 2005, calculation was by Z. Knezevic and A. Milani. </p> The top left plot is a slightly modified reduced version of <a href="https://en.wikipedia.org/wiki/Image:Asteroid_proper_elements_i_vs_a.png" class="extiw" title="en:Image:Asteroid proper elements i vs a.png">:Image:Asteroid_proper_elements_i_vs_a.png</a>. |
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