Dynamics of Polar Jets from the Chromosphere to the Corona: Mass, Momentum and Energy Transfer

Transcription

1 Dynamics of Polar Jets from the Chromosphere to the Corona: Mass, Momentum and Energy Transfer Judit Szente 1, Gabor Toth 1, Ward Manchester 1, Bart van der Holst 1, Enrico Landi 1, C Richard DeVore 2, Tamas Gombosi 1 (1) University of Michigan Ann Arbor (2) NASA Goddard Space Flight Center Fall AGU SH23D- 05 SPA- Solar and Heliospheric Physics Tuesday, December 15, 2015 This work was supported by the NSF grant AGS The research leading to these results was partly funded by the European Union s Horizon 2020 research and innovation program under grant agreement No PROGRESS.

2 Why Coronal Jets are InteresTng? MagneTc Field Topology Coronal HeaTng ReconnecTon Solar Wind OuWlow

3 Goal of this study Study transport due to jet energy, momentum, mass interacton with local plasma State of the art model physically well- established two temperature coronal model: AWSoM full 3D MHD corona (24 R ) fully resolved small- scale jet structure (0.013 R ) [Solar Radii] Grid structure across the jet region [Solar X Radii] Cell size: 1000 km in azimuthal, 20 km in radial direc5on Magne5c field strength [G]

4 GLOBAL: Solar wind model Chromospheric inner- boundary Ambient dipole: G at pole Coronal heatng and solar wind acceleraton via Alfvén waves Model Setup LOCAL: Jet model Radial bipole under the surface RotaTng boundary conditon around bipole axis MagneTc lattude determines background field: open vs. closed This talk focuses on polar jets. Jet Model Parameters Strength at 1 R 70 G Radius of rota5on R Maximum speed 30 km/s

5 Radial and out- of plane velocity profile across the center of the jet Radial velocity with magne5c field Out- of plane velocity with magne5c field

6 Large scale velocity profiles (24 R ) (t = s) Radial velocity Out- of plane velocity V_r [km/s] V_y [km/s]

7 Large scale velocity profiles (24 R ) (t = s) Radial velocity Out- of plane velocity V_r [km/s] V_y [km/s]

8 Signatures in the magnetc field B=0 contour (color indicates proton temperature) Rela5ve change in magne5c energy Rela5ve change in azimuthal magne5c field

9 EnergeTcs in the jet s core ΔE [1e30 erg] Energy in Box [1e30 erg] 0.3 Total Energy 0.2 Magne5c Energy Gravita5onal Energy 0.1 Kine5c Energy Simulation Time [s] the ion and electron temperatures show significant differences in the jet region magnetc energy is dominant in the core periodic changes

10 Mass, momentum and energy transfer through the jet into the corona Δm [10 12 g] simulation time [s] Δmv 11 [10 12 g cm/s] MASS TRANSFER g/s 0.25 ΔE [1e30 erg] TOTAL ENERGY TRANSFER erg/s Gravita5onal Energy Kine5c Energy MOMENTUM TRANSFER g- cm/s simulation time [s] Magne5c Energy Total Internal Kinetic Magnetic Gravitational Simulation Time [s] magnetc energy is dominant only in the beginning gravitatonal energy change is dominant mass and momentum transport is significant compared to region with no jet

11 EnergeTcs of the jet Local Scale: Global Scale: ΔE [10 30 erg] 0.10 Jet core ΔE [10 30 erg] 0.6 Total Jet Magne5c energy change Gravita5onal+Internal +Kine5c energy change Gravita5onal+Internal +Kine5c energy change Magnetic Internal+Kinetic+Gravitational Simulation Time [s] Magne5c energy change Magnetic Internal+Kinetic+Gravitational Simulation Time [s]

12 Comparison of X- ray synthetc images to Hinode- XRT observatons shows similarites t = 01:03:30 simulaton Tme T13:13:07 foot point brightening dome of mixed temperature plasma foot point brightening dome of mixed temperature plasma plasma jet plasma jet same color scale same spatal scale also simulated AIA s EUV bands

13 Conclusions The modeled jet compares well with observatons. Inside perturbed corona up to 24 R (relatve to inital value) energy transport: erg/s (12% increase in 3 hours) momentum transport: g- cm/s 2 (102% increase in 3 hours) mass transport: g/s (55% increase in 3 hours) Small local phenomena like a jet can produce global effects. We predict observable signatures for Solar Probe Plus.