24
Flux ropes in space plasmas Alexey Isavnin Department of Physics University of Helsinki, Finland Lectio praecursoria, 14 August 2014

Lectio Praecursoria from PhD defence (2014)

Embed Size (px)

Citation preview

Page 1: Lectio Praecursoria from PhD defence (2014)

Flux ropes in space plasmas Alexey Isavnin

Department of Physics University of Helsinki, Finland

Lectio praecursoria, 14 August 2014

Page 2: Lectio Praecursoria from PhD defence (2014)

“If I had to choose a religion, the Sun as the universal giver of life would be my god.”

Napoleon Bonaparte

“Neither the Sun nor death can be looked at steadily.”

François La Rochefoucauld

Page 3: Lectio Praecursoria from PhD defence (2014)

Outline

•  Space weather: Sun–Earth connection, its mechanism and effect on us

•  Coronal mass ejections: multipart configuration and embedded flux ropes

•  Evolution of solar flux ropes: deflections and rotations •  Magnetospheric flux ropes: evolution and substorm

dynamics

1/18

Page 4: Lectio Praecursoria from PhD defence (2014)

Space weather

2/18

Space weather describes the conditions in space that affect Earth and its technological systems

Page 5: Lectio Praecursoria from PhD defence (2014)

Space weather. Spectacular…

3/18

Page 6: Lectio Praecursoria from PhD defence (2014)

Space weather. Spectacular…

4/18

Page 7: Lectio Praecursoria from PhD defence (2014)

Space weather. Spectacular but hazardous

5/18

Page 8: Lectio Praecursoria from PhD defence (2014)

Space weather. How does it work

6/18

Coronal mass ejections (CMEs) are the drivers of the strongest geomagnetic storms. Geoffective CME is the one that caused geomagnetic disturbance.

Page 9: Lectio Praecursoria from PhD defence (2014)

Space weather. How does it work

7/18

1 2

3 4

Page 10: Lectio Praecursoria from PhD defence (2014)

Flux rope CMEs and their internal structure

Page 11: Lectio Praecursoria from PhD defence (2014)

Magnetic flux ropes

8/18

•  Local cylindrical geometry •  Helical magnetic field lines with zero twist in the core and

increasing with the distance from the axis •  Maximum magnetic field strength along the axis

Page 12: Lectio Praecursoria from PhD defence (2014)

Coronal mass ejection

9/18

CMEs are not just explosions on the Sun but eruptions of magnetic flux ropes.

Page 13: Lectio Praecursoria from PhD defence (2014)

Five-part CME structure

10/18

The dark cavity represents the flux rope. Bright core is the prominence material. Faint loop is the signature of a shock wave driven by the CME.

Page 14: Lectio Praecursoria from PhD defence (2014)

Conclusions

11/18

•  CMEs and ICMEs are both multipart structures with five distinct parts distinguishable.

•  Flux rope occupies the dark cavity area of a CME observable in white light.

•  Front and rear ICME parts originate near the Sun and correspond to piled-up material (bright loop) in front of the flux rope and prominence material (bright core), respectively.

•  Sheath region region form during fast CME propagation and occupies the region of diffusive emission.

Page 15: Lectio Praecursoria from PhD defence (2014)

Evolution of solar flux ropes

Page 16: Lectio Praecursoria from PhD defence (2014)

Solar flux rope evolution

•  Expansion •  Deflection •  Rotation •  Distortion

Motivation: Change of flux rope orientation can result in change of geomagnetic effectiveness. Important for space weather forecasting.

12/18

Page 17: Lectio Praecursoria from PhD defence (2014)

Tracking a flux rope requires several tools

13/18

0 Rs 5 Rs 20 Rs 1 AU

solar disk observations coronagraph imaging in-situ measurements

Page 18: Lectio Praecursoria from PhD defence (2014)

Conclusions

14/18

•  Flux ropes continuously deflect towards the solar equatorial plane during their travel from the Sun to the Earth’s orbit.

•  Flux ropes rotate while getting approximately aligned with heliospheric current sheet.

•  Geometrical evolution of ejected flux ropes in the inner heliosphere was found to be caused by magnetic interaction with Parker-spiral-structured solar wind.

•  60% of flux rope evolution happens during the first 14% of their travel distance from the Sun to 1 AU.

Page 19: Lectio Praecursoria from PhD defence (2014)

Evolution of magnetospheric flux ropes

Page 20: Lectio Praecursoria from PhD defence (2014)

Magnetospheric substorm dynamics

15/18

1.  Energy from the solar wind due to interaction with magnetic structures within is stored as excess magnetic flux in the magnetosphere.

2.  A reconnection site (X-line) is formed in the magnetotail. 3.  During the explosive substorm reconnection part of excess

energy is released tailwards and part is dissipated in the ionosphere increasing auroral luminosity.

Page 21: Lectio Praecursoria from PhD defence (2014)

Plasmoid formation

16/18

Plasmoid is a flux-rope-like structure formed between N2 and N3 X-lines. It carries away the excess energy from the magnetosphere.

Page 22: Lectio Praecursoria from PhD defence (2014)

Multiple X-line reconnection

17/18

Due to plasma instabilities multiple X-lines can be dynamically generated at the near-Earth reconnection site. Flux ropes formed in between the X-lines can be released both tailwards and Earthwards.

Page 23: Lectio Praecursoria from PhD defence (2014)

Conclusions

18/18

•  Multi-X-line sites are dynamic regions and result from plasma instabilities. Flux ropes can be formed and ejected sequentially from these areas both tailwards and Earthwards.

•  The properties of released flux ropes reflect solar wind conditions and their change correspond to reconfiguration of the magnetosphere.

•  Earthward moving flux rope get deteriorated due to anti-reconnection and eventually degrade into dipolarization fronts.

Page 24: Lectio Praecursoria from PhD defence (2014)

Thanks for your attention!