after Woch et al., 1997

700-800 km/s 400 km/s after Woch et al., 1997

Slow solar wind from an equatorial coronal hole Slow solar wind from a polar coronal hole

Low-speed wind models Helmet-streamer Blob-loop reconnection Wang et al. (1999) Expanding active region Nakagawa & Uchida

Relation between speed and coronal hole area The speed of the solar wind scales with the coronal hole area. [Nolte et al., 1976] Intermediate and slow streams originated in smaller coronal holes at low latitudes and from open field regions just outside coronal hole boundaries. [Neugebauer et al., 1998]

Wang & Sheely model Magnetic field configuration smaller expansion high speed larger expansion low speed RADIAL DISTANCE after Wang and Sheeley, 1990

from flux expansion factor in situ observation after Wang and Sheeley, 1990

potential field neutral line A neutral line does not traverse through the minimum speed locus. after Crooker et al., 1997

Slow SW from an equatorial small CH

potential field neutral line ? ? after Kojima et al., 1999

after Kojima et al., 1999

Hinode Continuous Upflow of Plasmas (Ti/Poly Filter)

MHD simulation by Linker & Mikic ’99 V V N low density low speed from coronal hole

after Kojima et al., 1999 Coronal hole model Helmet streamer model

potential field neutral line A neutral line does not traverse through the minimum speed locus. after Crooker et al., 1997

V Np φB

V Np To 106K

V Np Na/Np

Solar Wind in CR 1897 (June 12 – July 10, 1995) Parameter Slow (HPS) Slow (seCH) Fast (leCH) VP [km/s] 343±12 323±9673±14 NP [cm-3] 11.7±3.3 10.2±0.6 3.2±0.5 TP [105 K] 0.39±0.14 0.55±0.112.20±0.39 TO [106 K] 1.85±0.24 1.99±0.191.42±0.13 Nα/ NP 0.009±0.003 0.031±0.0080.039±0.004

slow wind (SCH) coronal hole steady large

Origin of slow SW(seCH) Coronal hole origin but ⇒ extra momentum source in lower corona Large NV High To (in seCH) Enhanced Heating in lower corona seCH StrongB (in seCH)

Slow SW from a polar CH

dependence on polar coronal hole scale size 1999 1991 2000 Oct. 1999

SOHO/EIT 195 Å 1999/10/23 22:24 UT

Small Polar Coronal Hole

Wang & Sheely model Magnetic field configuration smaller expansion high speed larger expansion low speed RADIAL DISTANCE Energy/mass flux B=4～6 G Less magnetic energy after Wang and Sheeley, 1990

Polar Low-speed Solar Wind at Solar Activity Maximum of Cycle 23 October 23, 1999 Ohmi et al. [2002]

Polar Low-speed Solar Wind at Solar Activity Maximum of Cycle 22 June 27, 1990 Ohmi et al. [2001]

12G 4～6G 18G slower fast slower slow

Wang & Sheely model Magnetic field configuration smaller expansion high speed larger expansion low speed RADIAL DISTANCE Energy/mass flux after Wang and Sheeley, 1990

Magnetic Field in the Coronal Holes

Density excess in slow wind source 300～3000 The slowest SW has f = 100～1000.

after Woch et al., 1997

after Woch et al., 1997

Presentation Transcript

Raine et al (1997) Brain abnormalities in murderers

et al.

Dalton et al.

IBM Clustering: after Brown et al

Deschamps et al.

Branigan et al.

Raine et al (1997) Brain abnormalities in murderers

Youssef, et. al.

(After Taub et al – 1981)

Koepke et al., [1997] Kaufman and Tanre [1997] Levy et al., [2004] Remer et al., [2006]

Pangea, et al

NCCLS (1997) Approved standard M27-A. Rex JH et al. Clin Infect Dis (1997) 24:235-247.

Phase diagram of MnSi (after Pfleider er et al 2001)

CHO et al.

Effects of the 1997 El Nino (Chandra et al., GRL, 1998)

Leeman et al 2004 Moriguti et al 2004 Rosner et al 2003

Solute Mass Transfer in CRRT Garred et al., AJKD 1997

UNDERSTANDING ET AL

Lukasik et al, INDRA collaboration PRC55, 1906 (1997)

Ward et al. 1997, Nature 390:131-132