luhmann1 an nsf science and technology center led by boston university, involving solar partners at...
Post on 22-Dec-2015
215 views
TRANSCRIPT
![Page 1: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/1.jpg)
Luhmann1
An NSF Science and Technology Center led by Boston University, involving solar
partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL, and UCB
CISM’s solar/heliospheric science goals center on thedevelopment of a validated, coupled, modular, simulation of the Sun to L1 space, including:
-> a realistic corona and resulting solar wind structure
-> realistic CME initiation and propagation capability
-> a SEP injection and transport scheme that uses the MHD model results
-> solar wind and SEP coupling to geospace
![Page 2: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/2.jpg)
Luhmann2
InnerMagnetosphere
The CISM Coupled Modeling
Solar Corona SAIC
Solar Wind ENLIL Ionosphere
T*GCM
Active Regions
SEP
Ring Current
Radiation Belts
Geocorona and Exosphere
Plasmasphere
MI Coupling
MagnetosphereLFM
Solar CISM
![Page 3: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/3.jpg)
Luhmann3
key areas of progress toward the solar-heliosphere simulations to date
->Developed CORHEL, a coupled MAS (SAIC) corona/ ENLIL (U of Colorado) solar wind MHD simulation with user-friendly interface. Validation is currently underway
-> Carried out an initial, coupled, modular, end-to-end (Sun to Middle Atmosphere) proof-of-concept simulation of an ad-hoc CME event- described in a special issue of JASTP
->Characterized details of realistic CME initiation in selected observations, especially May 12, 1997
- >Adopted a “Cone” Model of CME events for developing a generalized first-order scheme and for interplanetary propagation and SEP code development
![Page 4: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/4.jpg)
Luhmann4
key goals in solar/heliosphere areas
-> Archived Codes capable of providing regular MHD simulations of the quiet corona and solar wind, with documented performance
->An archived Cone Model simulation code for CME events, including an integrated SEP code module
-> Documented schemes for observation-based CME initiation and evolution in the inner heliosphere
-> Archived Codes for coronal/solar wind/SEP event simulations for examples with realistic CME initiation
->A geospace coupler scheme for solar wind, shocks and SEPs
![Page 5: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/5.jpg)
Luhmann5
CISM Solar/Heliospheric Code Computational Grids
L1
Coupled MAS corona, ENLIL solar wind
MAS corona grid showing magnetic field lines and solar magnetogram- based boundary field ( high spatial resolution segment option for active region resolution)
![Page 6: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/6.jpg)
Luhmann6
Much effort has been expended in evaluating and improving the synoptic field maps used as the inner boundary conditions (e.g. polar corrections)
Full-disk data from SOHO MDI or ground based observatories provide most raw data although localized vector mag data are also examined (e.g. CORHEL currently uses NSO, WSO)
Models use synoptic Field map(s) including: traditional 27-day Carrington, updating fields, or high cadence updating insets
![Page 7: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/7.jpg)
Luhmann7
Both in-situ L1 solar wind data comparisons and coronal hole observations are being used to validate the CORHEL simulations of the steady corona and
solar wind-The results are sensitive to the details of the synoptic maps used.
(D. Odstrcil images)
![Page 8: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/8.jpg)
Luhmann8
e.g. Low latitude hole sources depend on boundary map and code resolution
![Page 9: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/9.jpg)
Luhmann9
synoptic map and CORHEL plans
-> CORHEL is being validated against L1 data sets and compared to results from the WSA semi-empirical model and a “hybrid” Model with WSA corona and ENLIL solar wind
->Improved solar wind heating/acceleration is being added (MAS in current CORHEL version is polytropic)
-> CORHEL is being expanded to use a greater variety of synoptic map options (used synoptic maps are part of validated codes)
-> Synoptic map treatments, in particular polar corrections and updates are being tested for performance as boundary conditions
![Page 10: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/10.jpg)
Luhmann10
The Halo CME on May 12, 1997 and its associated interplanetary consequences are being used to
develop a CISM approach to realistic event simulation
Photospheric field from SOHO MDI
SOHO EIT EUV observations
SOHO LASCO C2 and C3 observations
![Page 11: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/11.jpg)
Luhmann11
A useful aspect ofthis event was theobservation of similarCMEs on both limbsinvolving the sameactive region
Left to right: May 5,May 12 halo, May 16CMEs (SOHO imagesFrom S. Yashiro’sCDAW CME catalog)
![Page 12: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/12.jpg)
Luhmann12
The active region magnetic field evolution was closely examined as well as other signatures of a potentially eruptive site including H-alpha
(Y. Li figure)
![Page 13: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/13.jpg)
Luhmann13
A force-free field model (left) was used to reproduce an SXT soft x-ray image. The PFSS model (above right) suggested the larger scale
field context and global connections of the active
region. (from Y Liu and Y Li)
May 12, 04:34 UT
SOHO EIT Images
![Page 14: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/14.jpg)
Luhmann14
From Y. Li
Local Correlation Tracking was used to infer the activeregion horizontal velocities
![Page 15: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/15.jpg)
Luhmann15
Inferred flows parallel to and perpendicular to the active region neutral line were found to exhibit shear and convergence, respectively, as required by CME initiation scenarios
Above: a horizontal cut through the center of the sunspot along which flows are evaluated.
Right- spatial profile of the horizontal velocity component that is perpendicular (Vperp) and parallel (Vpara) to the neutral line (NL)
![Page 16: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/16.jpg)
Luhmann16
Vortical velocity fields were applied to a bipolar active region in an MHD simulation to produce shear along the neutral line……
Figures from Y Liu (left), J Linker and Z Mikic (right)
![Page 17: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/17.jpg)
Luhmann17
To produce a field line structure resembling the force-free field and the SXT image of the active region………….
![Page 18: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/18.jpg)
Luhmann18
When evolved within the global background field deduced from the observations, followed by flux cancellation (reduction) in the active region, eruption occurs……..
Br from Potential field for Model flux and MDI data at r = 1.121 Rs
Images from Z. Mikic and J. Linker
![Page 19: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/19.jpg)
Luhmann19
Still needed: addition of solar wind, interplanetary transport
![Page 20: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/20.jpg)
Luhmann20
Geometrical and kinematical fitting:provides latitude, longitude, angular width, and velocity (D. Odstrcil and
X. Zhao figures, LASCO data)
The CME Cone Model –alternative reintroduced by Zhao et al. (2002)
![Page 21: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/21.jpg)
Luhmann21
May 12, 1997 Cone Model boundary conditions based on MAS model properties at 30 Rs (Cone Model runs in the ENLIL domain)
Running difference images fitted by the cone model(D. Odstrcil image)
![Page 22: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/22.jpg)
Luhmann22
Cone Model, May 12, 1997 CME event………..
Fast stream follows the ICME(D. Odstrcil image)
![Page 23: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/23.jpg)
Luhmann23
Cone Model details-density contours and interplanetary field lines
(D. Odstrcil image)
![Page 24: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/24.jpg)
Luhmann24
Simulated Cone Model in-situ parameters at 1 AU are compared to WIND observations on May 12-22, 1997………………..
(D. Odstrcil image)
![Page 25: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/25.jpg)
Luhmann25
More complex cases of cone model runs are being examined (here, May, 1998 multiple CMEs), illustrating challenges ahead……..
Four halo CMEs between April 29 and May 2, 1998
( Work in progress )
(D. Odstrcil figure)
![Page 26: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/26.jpg)
Luhmann26
Snapshots of observer-connected MHD simulation field lines are saved to locate and characterize the shock source of SEPs
(Figure from S. Ledvina)
![Page 27: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/27.jpg)
Luhmann27
SEP 10-100 MeV proton time profiles are calculated in a post-process mode using saved MHD field lines and shock parameters
2.1-2.5 MeV H
19-22 MeV H
~2 MeV He
IMP-8
(data plot from A. Tylka) Sample calculated profile
![Page 28: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/28.jpg)
Luhmann28
Ion kinetic hybrid code results will eventually be used to create a physics-based shock source description……………..
Ion Distributions: quasi-parallel case
(figure from D. Krauss-Varban)
![Page 29: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/29.jpg)
Luhmann29
Geospace coupling is currently single ENLIL grid point-based
ICME
SHOCK
L1-EARTH
![Page 30: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/30.jpg)
Luhmann30
Simulated Solar Wind Parameters at L1
Result in driven CISM geospace model responses including high
latitude energy input (inset).
From D. OdstrcilFrom M. Wiltberger
![Page 31: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/31.jpg)
Luhmann31
Simulated Solar Wind Parameters at L1
…and SEP access to the magnetosphere and polar cap
From D. Odstrcil From M. Hudson, B. Kress
![Page 32: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/32.jpg)
Luhmann32
event simulation plans
-> The Cone Model will be developed into a CORHEL-like general use code for “cone modeled” transients and validated, with a post-process SEP model
-> The May 12, 1997 CME realistic initiation case will be completed (solar wind added, propagation to Earth, SEP event model) and validated
-> Experiments with other initiation schemes and case studies are underway and will follow the May ’97 event path
-> CISM collaborations are encouraged!
![Page 33: Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,](https://reader035.vdocument.in/reader035/viewer/2022062516/56649d7f5503460f94a62bd2/html5/thumbnails/33.jpg)
Luhmann33
CISM has benefited from the Solar MURI Program Center at UCB -e.g.theapproach to observation-driven eruptionsthrough Local Correlation Tracking
Collage of Solar MURI results,From Bill Abbett