PMID- 23518616
OWN - NLM
STAT- PubMed-not-MEDLINE
DCOM- 20141126
LR  - 20240322
IS  - 2193-1801 (Print)
IS  - 2193-1801 (Electronic)
IS  - 2193-1801 (Linking)
VI  - 2
IP  - 1
DP  - 2013 Dec
TI  - Large-scale solar magnetic field mapping: I.
PG  - 21
LID - 10.1186/2193-1801-2-21 [doi]
LID - 21
AB  - This article focuses on mapping the Sun's large-scale magnetic fields. In 
      particular, the model considers how photospheric fields evolve in time. Our solar 
      field mapping method uses Netlogo's cellular automata software via algorithms to 
      carry out the movement of magnetic field on the Sun via agents. This model's 
      entities consist of two breeds: blue and red agents. The former carry a fixed 
      amount of radially outward magnetic flux: 10(23) Mx, and the latter, the 
      identical amount of inward directed flux. The individual agents are 
      distinguished, for clarity, by various shades of blue and red arrows whose 
      orientation indicates the direction the agents are moving, relative to the 
      near-steady bulk fluid motions. The fluid motions generally advect the field with 
      the well known meridional circulation and differential rotation. Our model 
      predominantly focuses on spatial and temporal variations from the bulk fluid 
      motions owing to magnetic interactions. There are but a few effects that agents 
      have on each other: i) while at the poles, field agents are connected via the 
      Babcock - Leighton (B - L) subsurface field to other latitudes. This allows them 
      to undertake two duties there: A) the B - L subsurface field spawns the next 
      generation of new magnetic field via new agents, and B) the B - L subsurface 
      field attracts lower-latitude fields via the "long-range" magnetic stress 
      tension; ii) nearby agents affect each other's motion by short-range 
      interactions; and iii) through annihilation: when opposite field agents get too 
      close to each other, they disappear in pairs. The behavior of the agents' long- 
      and short-range magnetic forces is discussed within this paper as well as the 
      model's use of internal boundary conditions. The workings of the model may be 
      seen in the accompanying movies and/or by using the software available via 
      SpringerPlus' website, or on the Netlogo (TM) community website, where help is 
      readable available, and should all these fail, some help from the author.
FAU - Schatten, Kenneth H
AU  - Schatten KH
AD  - Ai-solutions, Inc, Suite 215 10001 Derekwood Lane, 20706 Lanham, MD USA.
LA  - eng
PT  - Journal Article
DEP - 20130123
PL  - Switzerland
TA  - Springerplus
JT  - SpringerPlus
JID - 101597967
PMC - PMC3601253
OTO - NOTNLM
OT  - Heliosphere
OT  - Magnetic fields
OT  - Solar activity
OT  - Solar dynamo
OT  - Solar-terrestrial
OT  - Sun
OT  - Sunspots
EDAT- 2013/03/23 06:00
MHDA- 2013/03/23 06:01
PMCR- 2013/01/23
CRDT- 2013/03/23 06:00
PHST- 2012/08/31 00:00 [received]
PHST- 2012/11/16 00:00 [accepted]
PHST- 2013/03/23 06:00 [entrez]
PHST- 2013/03/23 06:00 [pubmed]
PHST- 2013/03/23 06:01 [medline]
PHST- 2013/01/23 00:00 [pmc-release]
AID - 134 [pii]
AID - 10.1186/2193-1801-2-21 [doi]
PST - ppublish
SO  - Springerplus. 2013 Dec;2(1):21. doi: 10.1186/2193-1801-2-21. Epub 2013 Jan 23.