Dust particles from 141P/Machholz 2?

Peter Bus


On August 13, 1994 Donald E. Machholz discovered a new short periodic comet with a period of approximately 5,23 years. Shortly after the discovery it was realised that the comet has recently (within years) split up into a number of fragments. The comet passed perihelion at 0,75AE on September 18, 1994 and passed descending node at October 4.
Earth reached this point some 55 days later on November 28, 1994 at 14h UT at a distance of 0,186 AE at the outside of the comets orbit. This distance is too large for high meteor activity, but some particles could enter the earth atmosphere.
The computed position of the Radiant is situated near the triple-point Ophiuchus-Hercules-Aquila roughly at about RA 18h30m; DC +11 degrees which is about 20 degrees west of Altair. One should pay attention with a large zenithal attraction due to the low velocity of 19 km/sec of possible meteors emerging from comet 141P/Machholz 2.
On November 27, 28 and 29, 1994, between 12 and 16h UT, meteor scatter observations were carried out. Results are presented in the figure below.



Hourly radio rates as recorded on November 27, 28 and 29, 1994. The squares represent hour rates per 30-minute intervals on November 28. The diamonds represent the mean hour rates per 30-minute intervals on November 27 and 29. The error bars represent 1-sigma errors. The dots represent the uncorrected net values on November 28 per 30-minute intervals. The error bars represent 1-sigma errors with the errors of November 27 and 29 taken into account.
Around nodal passage on November 28, 1995 no enhanced activity is monitored.

This figure shows the mean activity on November 27 and 29, 1994 at about 75 meteors/hour and the activity reached even higher values on November 28. It seems evident the enhanced activity is caused by particles emerging from comet 141P/Machholz 2.

This conclusion is even more stressed through:

  1. Maximum activity is observed around nodalpassage.
  2. The uncorrected counts are in good agreement with the radio observability function, which has been computed for the theoretical radiant.

But is this a valid conclusion?

  1. Coincidence could play a large role here.
  2. Only a few long-duration reflections have been observed.
  3. No visible observations are known.
  4. Calculations by Asher & Steel suggest particles could not intersect with earth orbit or only those emerging with high velocity from the comets surface.

We therefore suggest in case of an upcoming return, to observe with all possible means such as video, photographic and visual and above all small wide-field telescopes.

In 1999 we again have the opportunity to observe possible streammembers of this comet. The comet passes perihelion on December 9, 1999 and reaches descending node on December 25, 1999. Earth passes this point about 27 days earlier on November 28, 1999 almost exactly at 20h00m UT at 0,1897 AE distance outside the comets orbit. The moon rises at 21h32m UT and will not interfere observations because the theoretical radiant has set one hour before. At 17h UT the astronomical twilight starts and the theoretical radiant is 31 degrees above the southwestern horizon.


Theoretical Radiant, November 28
RA = 18h30m; DC = +11
Groningen, the Netherlands
53.2 N ; 6.5 E
TimeElevationAzimuth
(S=180)
(UT)(degrees)(degrees)
16h30m36236
16h45m33240
17h00m31244
17h15m29247
17h30m27251
17h45m25254
18h00m23257
18h15m21260
18h30m18263
18h45m16267
19h00m14270
19h15m12273
19h30m10276
19h45m7279
20h00m5282
20h15m3285
20h30m1288


Finderchart Theoretical Radiant at RA = 18h30m ; DC = +11


Literature:

  1. D.J.Asher and D.I.Steel, Mon. Not. R. Astron. Soc. 280, 1201-1209 (1996)
  2. Bus, E.P., Radiant 16, nr. 5, pp. 125 (1994)
  3. Bus, E.P., Radiant 16, nr. 6, pp. 143 (1994)
  4. IAUC 6053, 6066, 6070, 6071 en 6081 (1994)
  5. IAUC 7231 (1999)
  6. Jenniskens, P., personal communications (1994)
  7. MPC 35815 (1999)




Back to
DMS homepage
back.gif This page was last modified on October 29, 1999 by
Peter Bus and Casper ter Kuile