Extreme Space Weather Events [email protected] th June 2014 The Maunder minimum: An...
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Extreme Space Weather Events workshop [email protected].uk 9 th June 2014 The Maunder minimum: An extreme space climate event? Mathew Owens, Mike Lockwood, Luke Barnard, Chris Scott and Ken McCracken The Maunder minimum: An extreme space climate event
Extreme Space Weather Events [email protected] th June 2014 The Maunder minimum: An extreme space climate event? Mathew Owens, Mike Lockwood,
Extreme Space Weather Events [email protected]
th June 2014 The Maunder minimum: An extreme space climate event?
Mathew Owens, Mike Lockwood, Luke Barnard, Chris Scott and Ken
McCracken The Maunder minimum: An extreme space climate event
Slide 2
2 Overview Direct observations Sunspots Aurora Cosmogenic
isotope abundance Climate observations Reconstructions Geomagnetic
Sunspot Solar wind speed Space weather implications
Slide 3
The Maunder minimum Eddy, Science, 1976 A period 1645-1715
with: An absence of sunspots An (apparent) reduction in auroral
activity An (apparent) reduction in coronal structure during
eclipses A reduction in 14 C, suggesting increased cosmic ray flux
( 10 Be is now known to have increased, though still cycled) 3
Slide 4
Sunspot number Hoyt and Schatten, Sol Phys, 1998; Lessu et al,
A&A, 2013; Svalgaard, IAU, 2011; Lockwood et al, JGR, 2014 4
Post 1750
Slide 5
Sunspot number: 11-year running means 5 Post 1750
Slide 6
Aurora e.g., Siscoe, Rev Geophys, 1980 6
Slide 7
Cosmogenic isotope abundance Steinhilber et al., PNAS, 2011
7
Slide 8
Heliospheric modulation potential Steinhilber et al., PNAS,
2011 8
Slide 9
Climate records Manley, QJRMS, 1974, Lockwood et al., ERL, 2011
9 No little ice age.
Slide 10
Open Solar Flux, F S Flux threading the coronal source surface
Unsigned Flux, F U = |B R | r 2 cos( ) d d r = heliocentric
distance B R = radial field = solar latitude = solar longitude + /2
2 - /2 0 closed field line open field lines
Slide 11
Ulysses Balogh et al., 1995; Smith et al., 2001; Lockwood et
al., 2000 ecliptic Ulysses showed that everywhere |B R |(d/R) 2 =
|B RE | Thus total unsigned magnetic flux leaving the sun = 4 R 2
|B RE | |B RE | Earth R d |B R |
Slide 12
Geomagnetic reconstructions Lockwood et al., JGR, 2014. See
also Svalgaard & Cliver, JGR, 2010 12
Slide 13
Relation of F S and V SW Lockwood & Owens, JGR, 2014
13
Slide 14
Relation of F S and V SW Lockwood & Owens, ApJ, 2014;
Cliver & Ling, Sol Phys, 2011 14
Slide 15
Before 1845: F S from R Solanki et al., Nature, 2000; Owens
& Crooker, JGR, 2006 F S can be modelled as a continuity
equation dF S /dt = S L F S S ~ f CME ~ R 15
Slide 16
Loss of F S Sheeley & Wang, ApJ, 2001; Owens et al., JGR,
2011 16
Slide 17
F S loss and the HCS tilt Owens and Lockwood, JGR, 2012 17
Slide 18
F S reconstruction Owens and Lockwood, JGR, 2012 18 F S sourceF
S loss
Slide 19
F S reconstruction Owens & Lockwood, JGR, 2012; Lockwood
& Owens, JGR, 2014 19 Post 1750
Slide 20
F S reconstruction (11-year) Owens & Lockwood, JGR, 2012;
Lockwood & Owens, JGR, 2014 20 Post 1750
Slide 21
Maunder minimum Owens, et al, GRL, 2012 21
Slide 22
Modelling streamer belt width Schwadron et al., ApJ, 2010;
Lockwood et al., JGR 2014 Separate streamer belt and coronal hole
fluxes: F S = F SB + F CH L = L SB + L CH Assume: New flux is
injected into the streamer belt Streamer belt flux eventually
becomes coronal hole flux Two coupled equations: dF SB /dt = S - L
SB F SB - S CH dF CH /dt = S CH - L CH F CH Streamer belt half
width = sin -1 [1-F CH /F S ] 22
Slide 23
Streamer belt width Owens et al., JGR 2014. See also Manoharan,
JGR, 2010 23 M. Druckmuller
Slide 24
Streamer belt width Lockwood and Owens, JGR, 2014 24 Post
1750
Slide 25
Space weather Great geomagnetic storms, Greenwich observatory
25
Slide 26
Maunder minimum summary Extremely low (long term) solar
magnetic field, compared to sunspot era and the last 10,000 years
Increased occurrence of cold winters, but no little ice age Reduced
auroral frequency, Difficult to quantify if this was extreme
Polarity of the solar field continued to cycle Coronal holes were
extremely small and the streamer belt was extremely broad Slow
solar wind at Earth. No/weak CIRs? Continued CME activity? 26
Slide 27
HCS location e.g., Smith el al., 2003; Owens & Forsyth,
LRSP, 2013 27
Slide 28
Computing the F S loss rate Owens and Lockwood, JGR, 2012
28
Slide 29
PFSS solutions Magnetic field polarity at coronal source
surface 29
Slide 30
Three-dimensional structure of interplanetary magnetic field
Owens et al., JGR, 2011 30
Slide 31
OCEANS STRATOSPHERE ( 2/3) GALACTIC COSMIC RAYS BIOMASS
TROPOSPHERE ( 1/3) ICE SHEETS 10 Be + AEROSOL ( ~1 year) ( ~1 week)
14 C 1/2 = 5370 yr = 2 atoms cm -2 s -1 10 Be 1/2 = 1.510 6 yr =
0.018 atoms cm -2 s -1 14 C & 10 Be: spallation products from
O, N & Ar 14 C+0 14 C0 ; 14 C0+0H 14 C0 2 + H
Slide 32
ERA-40 Analysis of DJF temperatures & circulation
(difference of high and low tercile subsets) sorted using open
solar flux F S Low solar activity gives lower surface temperatures
in central England Effect much stronger in central Europe Analysis
shows a distinct system to NAO (Woollings et al, GRL.,2010; see
also Barriopedro et al., JGR, 2008)
Slide 33
Space Challenges [email protected] Central England
Temperature (CET) Winter Means (DJF) show upward drift (linear)
rate of rise dT ann /dt = 0.37 C c -1
Slide 34
Space Challenges [email protected] Frost Fairs on the
Thames e.g. Winter 1683/4. Painted by Dutch artist Thomas Wijk
(1616-1677) N.B. notice how warm the next year was!
Slide 35
Space Challenges [email protected] Frost Fairs on the
Thames The last one was 1813/14. Painted by Luke Clenell (1781 1840
)
Slide 36
Space Challenges [email protected] Thames Freezing
Over N.B. in 1825 London Bridge demolished acted as a salt water
barrage plus embankment increased flow rate
Slide 37
Space Challenges [email protected] 1963 Thames at
Windsor Thames Freezing Over