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---+ Exoplanets and Sambridge et al. 

*%RED%Disclaimer: This is just an instant, superficial, analysis, not a serious, well thought-through analysis.%ENDCOLOR%*

A very rough quick analysis of Jean Schneider's Exoplanet database planetary mass distribution downloaded 2010-11-18, in response to request for an ultra-rapid comment on Sambridge et al. 2010, _"Benford's Law in the natural Sciences", Geophysical Research Letters,_ 37, L22301, which seems to be an extension of Sambridge et al. 2009, http://cdsads.u-strasbg.fr/abs/2009AGUFM.S33A1756S . 

There are 497 exoplanets in the list downloaded 2010-11-18, while Sambridge et al. 2010 had a list of 401 exoplanets from the same source, downloaded at some earlier date.

---++ rapid plots
Logarithmic binned distributions of masses, either in units of a Jupiter mass or of an Earth mass.
   * histJ.png: <br />
     <img src="%ATTACHURLPATH%/histJ.png" alt="histJ.png" width='360' height='252' />

   * histE.png: <br />
     <img src="%ATTACHURLPATH%/histE.png" alt="histE.png" width='360' height='252' />

Benford's Law distributions of masses, either in units of a Jupiter mass or of an Earth mass, with Poissonian error bars (whether or not these are valid requires more time for reflection...)
   * benJ.png: <br />
     <img src="%ATTACHURLPATH%/benJ.png" alt="benJ.png" width='360' height='252' />

   * benE.png: <br />
     <img src="%ATTACHURLPATH%/benE.png" alt="benE.png" width='360' height='252' />

Mass conversion used: Jupiter: 1.8986e27 kg, Earth: 5.9736e24,  so 1 Jupiter = 317.83 Earths.

---++ physical studies
   * Sambridge's "detection" (which they do not claim is significant) of somewhat more 6's than BL would seem to be qualitatively consistent with e.g.  Mordasini et al. ArXiv:0904.2542 who tested a planetary population model using just 32 observed planets. See Fig 2a, Fig 3, ArXiv:0904.2542 and compare to the above.

---++ instant summary
The present population of all detected exoplanets seems to consist of several narrow distributions, partly due to:
   * the use of several different methods (mostly radial velocities, transit, microlensing so far), which do not yet have much dynamic range, since the higher mass exoplanets are (usually) easier to detect for any given method; that is, each method gives a narrow log-distribution in masses
   * intrinsic distributions that have some narrow features in log(mass) - see e.g. Mordasini et al

Factors that are more likely to help smooth the distribution and make it more BL-like rather than less:
   * most of the exoplanets (radial velocity detections) are M sin _i_ estimates
   * "Exoplanet masses can be difficult to estimate"

For a more serious analysis, ask an exoplanet population specialist...

Topic attachments
I	Attachment	Action	Size	Date	Who
png	benE.png	manage	14.8 K	19 Nov 2010 - 11:52	BoudRoukema
png	benJ.png	manage	15.0 K	19 Nov 2010 - 11:52	BoudRoukema
png	histE.png	manage	13.0 K	19 Nov 2010 - 11:52	BoudRoukema
png	histJ.png	manage	13.0 K	19 Nov 2010 - 11:52	BoudRoukema

Topic revision: r1 - 19 Nov 2010, BoudRoukema

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