An Upper Limit for the Flux of Interstellar Dust Grains in the Solar System.

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A modeling technique is developed and used on spacecraft dust particle detector data to determine the interstellar component of the detected flux. The particle detectors used are those on Pioneers 8 and 9 (in solar orbit) and a similar instrument on the moon. The "front film" data are utilized. The modeling technique assumes various initial directions and velocities for the interstellar particles, traces them into the solar system to the detectors and predicts impact directions and fluxes as a function of time. Both impact direction and flux are found to show wide variations for a given set of initial parameters. The technique compares the predicted with the measured fluxes to arrive at a statistical determination of the interstellar component. The interstellar flux obtained by this technique is zero. From the statistical analysis significant upper limits are calculated for particles greater than or equal to 1.9 x 10('-14) gm (0.23 (mu)m diameter): 8.0 x 10(' -5) m('-2) s('-1) from the direction of local solar motion (270(DEGREES), 53(DEGREES)N ecliptic coordinates); 4.0 x 10('-5) m('-2) s('-1) from the direction of local interstellar wind (258(DEGREES), 4(DEGREES)N ecliptic coordinates); and values less than 8.0 x 10('-5) m('-2) s('-1) for other directions covering the whole sky. These limits apply to any interstellar dust stream having a velocity between 10 and 40 km s('-1) and having a ratio of radiation pressure to gravity of between 0 and 3/4.

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