## 4. Probability of detectionFrom the above modeling, we can evaluate the probability to detect a photometric stellar variation due to an extra-solar comet. We assume a survey of a given number of stars at a given accuracy. We carried out a large number of simulations of cometary occultations in all directions. ## 4.1. Orbital parametersThe characteristics of the comets are given by their distribution in the parameter space. Concerning the orbital parameters, the periastron density distribution is chosen to be the same as the one observed in the solar system: with AUAU (A'Hearn et al., 1995). Many sun-grazing comets have been discovered by SOHO with perihelion AU (Kohl et al. 1997; see also the numerous IAU Circulars). But it is still difficult to infer the distribution for these small periastrons. The above distribution is thus likely biased by an underestimate of the number of comets with small periastron, because such comets are difficult to observe. These star-grazing comets give a larger photometric variation. Therefore, we possibly slightly underestimate the probabilities of detection. We fixed all the apoastrons at 20 AU, the longitudes of periastron, the ascending nodes and the inclinations are chosen randomly. ## 4.2. Dust production rateOne of the most important parameter is the dust production rate. Because, it dictates the mass of dust in the tail, and constrains the detectability of the comet. The amplitude of the photometric variation is roughly proportional to that parameter. We consider that the dust production rate ( Finally, this distribution is normalized by , the number of comets per unit of time passing through the periastron with a production rate larger than . Hence, we have . Thus, ## 4.3. ResultsUsing a large number of various comets, we calculate the probability of detection at a given photometric accuracy. Then, the number of possible detections is simply this probability multiplied by , the duration of the observation and the number of stars surveyed . We suppose that the time scale between each measurement is small enough ( hour) that each variation above the detection limit will effectively be detected. As an example, we take year and , which is the order of magnitude for the future space mission COROT. The expected number of detections is plotted in Fig. 5. We
considered two types of planetary systems. The first one is similar to
the solar system with comets per
year with
kg s
The second type of planetary system is supposed to be a young
planetary system with a large cometary activity as during the youth of
the solar system. The typical example is the well-known star
Pictoris where comets' infalls
are commonly observed through UV and optical spectroscopy (see e.g.,
Ferlet et al. 1987, Lagrange et al. 1988, Beust et al. 1990,
Vidal-Madjar et al. 1994, 1998). For such a planetary system,
comets per year with
kg s The solar system is likely not exceptional. The bottom-line in Fig. 5 is a good estimate of the lower limit of the expected number of detections. Younger stars may have a higher level of activity, with a larger number of comets; but, although infrared excess have been observed around many main sequence stars, Pictoris is certainly a very peculiar case (Vidal-Madjar et al. 1998). Thus, the top-line in Fig. 5 gives a good estimate of the upper limit of the expected number of detections. Note that the major assumption that the dust production rates in
the solar system can be extrapolated to large values is realistic. A
large rate has effectively been observed in the recent comet Hale-Bopp
where it reached of few times
kg s It is very likely that in the near future a large number of extra-solar comets will be detected through occultations. For comparison, we also evaluate the probability to detect planets assuming that each star has a planetary system like the solar system. With an accuracy better than , Jupiter can be detected. Below , other giant planets are also detectable. But because of their large orbital periods, their contribution to the number of detections is smaller than the one from Jupiter. With a total probability of to detect a giant planet in one year, the survey of 30000 stars will give planets. With an accuracy better than , Earth-like planets start to be detectable. Because of their smaller distance to the star, they have larger contribution to the probability of planet detection. The Earth and Venus can be detected with a probability of in one year. Mars and Mercury, which are detectable with an accuracy of , give a total probability of . The comparison with the number of detection of comets shows that accurate photometric surveys should detect more comets than planets. © European Southern Observatory (ESO) 1999 Online publication: March 1, 1999 |