eCite Digital Repository
Precursors of the forbush decrease on 2006 December 14 observed with global muon detector network (GMDN)
Citation
Fushishita, A and Kuwabara, T and Kato, C and Yasue, S and Bieber, JW and Evenson, P and Da Silva, MR and Dal Lago, A and Schuch, NJ and Tokumaru, M and Duldig, ML and Humble, JE and Sabbah, I and Al Jassar, HK and Sharma, MM and Munakata, K, Precursors of the forbush decrease on 2006 December 14 observed with global muon detector network (GMDN), The Astrophysical Journal , 715, (2) pp. 1239-1247. ISSN 0004-637X (2010) [Refereed Article]
 | PDF Restricted - Request a copy 714Kb |
Copyright Statement
Copyright © 2010 The American Astronomical Society
Official URL: http://aas.org/
DOI: doi:10.1088/0004-637X/715/2/1239
Abstract
We analyze the precursor of a Forbush decrease (FD) observed with the Global Muon Detector Network on 2006 December 14. An intense geomagnetic storm is also recorded during this FD with the peak Kp index of 8+. By using the "two-dimensional map" of the cosmic ray intensity produced after removing the contribution from the diurnal anisotropy, we succeed in extracting clear signatures of the precursor. A striking feature of this event is that a weak loss-cone (LC) signature is first recorded more than a day prior to the storm sudden commencement (SSC) onset. This suggests that the LC precursor appeared only 7 hr after the coronal mass ejection eruption from the Sun, when the interplanetary (IP) shock driven by the interplanetary coronal mass ejection was located at 0.4 AU from the Sun. We find the precursor being successively observed with multiple detectors in the network according to the Earth's spin and confirmed that the precursor continuously exists in space. The long lead time (15.6 hr) of this precursor which is almost twice the typical value indicates that the interplanetary magnetic field (IMF) was more quiet in this event than a typical power spectrum assumed for the IMF turbulence. The amplitude (–6.45%) of the LC anisotropy at the SSC onset is more than twice the FD size, indicating that the maximum intensity depression behind the IP shock is much larger than the FD size recorded at the Earth in this event. We also find the excess intensity from the sunward IMF direction clearly observed during ~10 hr preceding the SSC onset. It is shown that this excess intensity is consistent with the measurement of the particles accelerated by the head-on collisions with the approaching shock. This is the first detailed observation of the precursor due to the shock reflected particles with muon detectors.
Item Details
| Item Type: | Refereed Article |
|---|---|
| Keywords: | cosmic rays - interplanetary medium - methods: data analysis - solar- terrestrial relations - Sun: coronal mass ejections (CMEs) |
| Research Division: | Physical Sciences |
| Research Group: | Astronomical and Space Sciences |
| Research Field: | High Energy Astrophysics; Cosmic Rays |
| Objective Division: | Expanding Knowledge |
| Objective Group: | Expanding Knowledge |
| Objective Field: | Expanding Knowledge in the Physical Sciences |
| UTAS Author: | Duldig, ML (Dr Marc Duldig) |
| UTAS Author: | Humble, JE (Dr John Humble) |
| ID Code: | 65511 |
| Year Published: | 2010 |
| Web of Science® Times Cited: | 15 |
| Deposited By: | Physics |
| Deposited On: | 2010-11-22 |
| Last Modified: | 2015-01-21 |
| Downloads: | 0 |
Repository Staff Only: item control page