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CSI 769-001/PHYS 590-001 Solar Atmosphere Fall 2004 Lecture 14 Dec. 08, 2004 Sun-Earth Connection and Space Weather.

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Presentation on theme: "CSI 769-001/PHYS 590-001 Solar Atmosphere Fall 2004 Lecture 14 Dec. 08, 2004 Sun-Earth Connection and Space Weather."— Presentation transcript:

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2 CSI 769-001/PHYS 590-001 Solar Atmosphere Fall 2004 Lecture 14 Dec. 08, 2004 Sun-Earth Connection and Space Weather

3 Today’s solar wind

4 Solar Wind Solar wind is a continuous outflow of solar particles, largely due to the thermal expansion of high temperature corona (~ 1MK). Due to the high thermal conductivity of coronal plasma, the solar atmosphere maintains high temperature even at large heliospheric distance, e.g., ~200,000 K at 1 AU. Because of this extended temperature distribution, the solar atmosphere maintains a finite thermal pressure even at large distance. Since the thermal pressure of the solar atmosphere can not be balanced by the external pressure (at large distance), the heliosphere can not be in a hydrostatic equilibrium; it expands.

5 Solar Wind (cont’d) The typical solar wind speed is about 400 km/s, which is consistent with Parker’s standard solar wind model that is based on hydrodynamic equations (see textbook section 10.1.2 at P.313) According to the model, wind speed of 400 km/s when base temperature of 1 MK

6 Solar Wind (cont’d) However, observations also show fast solar wind of speed 800 km/s Fast solar wind is found to be from coronal holes (and CMEs) Why coronal hole yields fast solar wind is still a mystery! It is not consistent with Parker’s standard thermal expansion model, because coronal hole has a cooler temperature and therefore a smaller expansion velocity according to the model There must be non-thermal energy deposition in solar wind in coronal hole regions

7 Solar Wind (cont’d) Solar wind speed distribution with heliospheric latitude Slow speed (400 km/s) in low latitude (e.g., < 20 degree) Fast speed (800 km/s) in high latitude (e.g,, > 20 degree)

8 Interplanetary Magnetic Field (IMF) The basic configuration: Parker Spiral Interplanetary magnetic field in the ecliptic plan

9 Interplanetary Magnetic Field (cont’d) Magnetic Field in the inner corona (< 2 Rs) is mainly closed loops

10 Interplanetary Magnetic Field (cont’d) Magnetic Field in the outer corona (> 2 Rs, but < 10 Rs) is radial

11 Interplanetary Magnetic Field (cont’d) Magnetic Field in the interplanetary space is spiral

12 Interplanetary Magnetic Field (cont’d) The spiral interplanetary magnetic field is caused by a combination effect of solar rotation and outward transport of magnetic field embedded with the spherical solar wind flow. Because of high electric conductivity, magnetic field is frozen-in with plasma in the corona and in the heliosphere. Solar magnetic field is carried away by solar wind flow due to frozen-in effect Solar wind flow is largely spherical along the radial direction Interplanetary space is a high β regime, the thermal pressure dominates the magnetic pressure; in other words, solar wind flow carries magnetic field with it.

13 Interplanetary Magnetic Field (cont’d) Well connected magnetic field from the Earth back to the solar surface at about west 57 degree For a typical solar wind of 400 km/s, it takes 104 hours or 4.3 days to reach the Earth During the same period, the Sun has rotated 57 degree (using a 27-day rotation period)

14 Interplanetary Magnetic Field (cont’d) Where is magnetically-well-connected solar region?

15 Interplanetary Magnetic Field (cont’d) The implications of magnetically-well-connected solar region. Impulsive SEP events, that are accelerated in flare regions, originate from a narrow region in western hemisphere, because particles move along the spiral field. When a coronal hole is present in the low latitude, fast solar wind shows in geo-space.

16 Interplanetary Coronal Mass Ejection (ICME) The counterpart of solar CME in interplanetary space. They are often caused by halo CMEs that are most likely to intercept the Earth’s orbit. Solar wind signature of ICME Shock interface Enhanced solar wind speed Enhanced magnetic field Magnetic cloud Enhanced plasma density Reduced proton temperature

17 ICME (cont’d) Solar wind signature of ICME

18 Space Weather in Geospace Earth Magnetic Field

19 Space Weather in Geospace Van Allen Belt: trapped energetic particles

20 Space Weather in Geospace Magnetosphere

21 Space Weather in Geospace The impact of ICME on magnetosphere

22 Space Weather in Geospace A geo-effective ICME usually has a sustained strong southern magnetic field Southern magnetic field is able to reconnect with the Earth magnetic field that is northern at the interface Reconnection at the magnetopause allow the reducing of magnetic shield of the Earth’s magnetosphere. As a result, solar wind energy and particles are dumped into the magnetosphere, causing geomagnetic storms

23 Space Weather in Geospace Ionosphere

24 Space Weather Effects Solar EM Radiation Due to solar flares No warning time Lasting short (tens of minutes) Scaled by NOAA GOES Soft X-ray magnitude Affect Ionosphere Solar Particle Radiation Due to flares and CMEs Short warning time (< 1 hr) Lasting long (hours to a few days) Scaled by particle monitor Direct impact with electronic and human objects Geomagnetic Storm Due to CMEs Possibly a few days warning time Lasting long (days) Scaled by Kp and Dst index Effect throughout the geo-space from ground to the entire magnetosphere

25 Space Weather Effects: NOAA Scale Five level scaling Level 5: Extreme Level 4: Severe Level 3: Strong Level 2: Moderate Level 1: Minor Solar EM Radiation: R1—R5 (Radio Blackouts) Solar Particle Radiation: S1—S5 (Solar Radiation Storm) Geomagnetic Storm: G1—G5 (Geomagnetic Storms)

26 Space Weather Effects: NOAA Scale Five level scaling Level 5: Extreme Level 4: Severe Level 3: Strong Level 2: Moderate Level 1: Minor Solar EM Radiation: R1—R5 (Radio Blackouts) Solar Particle Radiation: S1—S5 (Solar Radiation Storm) Geomagnetic Storm: G1—G5 (Geomagnetic Storms)

27 Space Weather Effects: NOAA Scale Solar EM Radiation: R5 HF Radio:Complete HF (high frequency**) radio blackout on the entire sunlit side of the Earth lasting for a number of hours. This results in no HF radio contact with mariners and en route aviators in this sector. Navigation: Low-frequency navigation signals used by maritime and general aviation systems experience outages on the sunlit side of the Earth for many hours, causing loss in positioning. Increased satellite navigation errors in positioning for several hours on the sunlit side of Earth, which may spread into the night side.

28 Space Weather Effects: NOAA Scale Solar Particle Radiation: S5 Biological: unavoidable high radiation hazard to astronauts on EVA (extra-vehicular activity); high radiation exposure to passengers and crew in commercial jets at high latitudes (approximately 100 chest x-rays) is possible. Satellite operations: satellites may be rendered useless, memory impacts can cause loss of control, may cause serious noise in image data, star-trackers may be unable to locate sources; permanent damage to solar panels possible. Other systems: complete blackout of HF (high frequency) communications possible through the polar regions, and position errors make navigation operations extremely difficult

29 Space Weather Effects: NOAA Scale Geomagnetic Storms: G5 Power systems: : widespread voltage control problems and protective system problems can occur, some grid systems may experience complete collapse or blackouts. Transformers may experience damage. Spacecraft operations: may experience extensive surface charging, problems with orientation, uplink/downlink and tracking satellites. Other systems: pipeline currents can reach hundreds of amps, HF (high frequency) radio propagation may be impossible in many areas for one to two days, satellite navigation may be degraded for days, low-frequency radio navigation can be out for hours, and aurora has been seen as low as Florida and southern Texas (typically 40° geomagnetic lat.)**.

30 Space Missions for Space Weather Solar Terrestrial Missions Operational Developmental Under Study Ulysses 90 ACRIMSAT 99 Cluster 00 CORONAS-F 01 FAST 96 Geotail 92 GENESIS 01 RHESSI 02 IMAGE 00 Polar 96 SAMPEX 92 SOHO 95 SORCE 03 TRACE 98 WIND 94 ACE 97 Voyager I & II 77 AIM 06 CINDI/CNOFS 04 CORONAS-PHOTON 06 COSMIC 05 EPOP 06 GEC >12 MC/DRACO >12 MMS 12 Radiation Belt Storm Probes 12 Picard 06-07 SDO 07 Solar-B 06 STEREO 05 Solar Orbiter 11 TWINS 04,05 Interhelioprobe 07-08 Iono-Thermosphere Storm Probes 10 SST 05 RESONANCE ? TIMED 01 SENTINELS 12-14 RAVENS 07 Solar Probe 12-14 Geospace Heliospheric Solar L5 Mission 08 Sich-1 04 Geostorm 09 SWISE 10-12 INTERBALL-PROGNOZ 06-07 THEMIS 06 STORMS 07 ROY/SCHWARM? Double Star 03/04 Auroral Quartet ?

31 STEREO Mission

32 (Trajectories) Tools & Services Science Data Facility Acquisition & Ingest Science User Sup http://spdf.gsfc.nasa.gov/ CDAWLib HelioWeb Data Environment

33 Summary Introduction Principles of Spectroscopy, Radiation Transfer Solar Missions and Instrumentation Solar Magnetic Field, Solar Cycle, and Solar Dynamo Lower Solar Atmosphere: Photosphere and Chromosphere Transition Region and Coronal Loop Dynamics (Midterm) Coronal Structure Coronal Plasma Properties, MHD Equations Ideal MHD, MHD Waves and Coronal Heating Solar Flare Filament Eruption and Coronal Mass Ejection Coronal Mass Ejection and Solar Energetic Particle (SEP) Sun-Earth Connection and Space Weather

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