Study of the April 20, 2007 CME-Comet interaction event with an MHD model Y. D. Jia 1, C. T. Russell 1, W. B. Manchester 2, K. C. Hansen 2, A. Vourlidas.

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Study of the April 20, 2007 CME-Comet interaction event with an MHD model Y. D. Jia 1, C. T. Russell 1, W. B. Manchester 2, K. C. Hansen 2, A. Vourlidas 3, L. Jian 1, M. R. Combi 2, T. I. Gombosi 2 1 IGPP/UCLA, Los Angeles, CA 2 University of Michigan, Ann Arbor, MI 3 Naval Research Laboratory, Washington EGU2008-A ST10 Monday, 14 April 2008

Introduction Disconnection events (DEs) are a class of violent disturbances in the cometary tails that can reveal dynamic information of the solar wind. In the past, only two types of structures are associated with DE triggering: Heliospheric current sheets (HCS) or shocks. In recent years, some CMEs are seen interacting with comets and causing DEs but never been fully understood. On April 20, 2007, STEREO SECCHI captured an outstanding event when a CME hit comet 2P/Encke at 0.34AU. This work is part of large-scale solar wind- comet interaction modeling effort as a cooperation between the Michigan CSEM and IGPP at UCLA :10 to the sun flux rope CME sheath

The April 20, 2007 Event The following reasons has made this event puzzling: Appear differently:  Evolve faster than most DEs, which lasts half a day  Show a longer gap between new and disconnected old tail.  Tail elongation with no tail rays Caused differently:  The dynamic pressure in this CME is not largely different from the ambient solar wind (<20%).  There are neither HCS crossings nor shocks associated [Vourlidas et al., 2007] HOW did this CME cause a tail disconnection? 18:10 18:50 19:30 20:10 6  10 6 km 2  10 6 km sheathFlux rope

Understanding the Appearances The long tail before this event suggest that the IMF vector is close to the x-z plane. The DE is initiated by a reversal of IMF primarily in the z direction. The new short tail is interpreted as caused by IMF turning into the x-y plane. 18:50 20:10 6  10 6 km x z B B Contour plots show typical appearances of a Halley sized comet [Jia et al., 2007]. Top: column density integrated perpendicular to the IMF place during a DE. Bottom: column density along the IMF direction.

MHD model 3-D simulation with the Michigan Block Adaptive-Tree Solar-wind Roe- type Upwind Scheme (BATS-R-US) code solving the ideal MHD equations. Photoionization, charge exchange, and dissociative recombinations are considered in the solar wind-comet interactions. 2.4  0.4  0.4 million km Cartesian grid based on the comet rest frame, x- axis points to the solar wind flow direction. Finest grid resolution is 25km, with a tail resolution of 2500km. X Y Z u comet uxux B

Steady State Solar wind values propagated from the magnetogram data at 2.5 solar radii using an MHD model [Cohen et al., 2008] Solar distance Gas production rate Q(#/s) B x (nT) B y (nT) B z (nT) u sw (km/s) n sw (#/cc) Ionization rate (s -1 ) 2P/Encke0.34AU 2.0   P/Halley1AU 7.0   BS (Mkm) CS (km) Encke Halley Subsolar distances of the bow shock and contact surface

Steady State contact surface region column density integrated perpendicular to the solar wind flow in the ecliptic plane B CD

Modeling the CME This is a relatively weak CME. The possibility of a flux rope to trigger the tail disconnection is tested in this work. The cross section of the flux rope is 100 times larger than the comet bow shock U SW X Z flux rope CME sheath 5Mkm(3Hours) Y Z Y Z U SW X Z flux rope CME sheath

Simplified flux rope The flux rope is represented by two stages of variations in the IMF: a reversal in B z and then gradually rotated into B y. The B x background is not applied for this preliminary study. B y max in this flux rope is estimated as 20nT.

2-d Projected Evolution BzBz Left: x-z plane cut with x=(-0.2,1.4) Right: x-y plane. black lines are field lines. red dashed line is the leading front of the CME, which is about to hit the comet The leading side of the CME outside the tail (marked by the dotted right red line) has been pushed more than 1  10 6 km but its remnant field in the comet tail is lagged behind at T=1:09h. The upwind B z start to drop below zero (left dotted red line) X [  10 6 km] 1

2-d Projected Evolution At 2:12h, the second reversal in B z starts to generate a plasmoid at x=0.4  10 6 km, as the B y component is decreasing the length of the tail in the x-z plane At 3:28 h, the plasmoid has been carried to x=0.9  10 6 km X [  10 6 km] 1

Reproducing the Appearances Column density along the y axis. Total time: 3:40 h

Summary This disconnection event in the comet tail at 0.34 AU is the effect of a CME, which is different from most recorded events in the past. The flux rope in this CME is the primary cause of the tail disconnection. The field reversals in the flux rope have caused the tail to disconnect, while the axial field has caused the new tail to appear short. By reproducing this event, we are able to infer the magnetic field configuration of this CME at 0.34AU.