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Advertisement. Helioseismology Summer School August 24 – August 28, 2010 Beijing Normal University Contact: Prof. Shaolan Bi Lecture Language: Mandarin. HMI Routine Helioseismology Results that You Can Download and Use. Junwei Zhao W. W. Hansen Experimental Physics Laboratory,

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Helioseismology Summer School

August 24 – August 28, 2010

Beijing Normal University

Contact: Prof. Shaolan Bi

Lecture Language: Mandarin


Hmi routine helioseismology results that you can download and use

HMI Routine Helioseismology Results that You Can Download and Use

Junwei Zhao

W. W. Hansen Experimental Physics Laboratory,

Stanford University, Stanford, CA94305-4085




1 routine production
1. Routine Production below the photosphere) flow maps and sound-speed perturbation maps for the following two types:

Input

Every 8 hours, we select 480-minute Doppler observations and make time-distance measurements. Inversions are done to derive subsurface flow fields and sound-speed perturbations. A total of 25 areas are selected and used to generate full-disk subsurface map.


1 routine production1
1. Routine Production below the photosphere) flow maps and sound-speed perturbation maps for the following two types:

Every 8 hours, we generate a nearly full-disk map.

For every Carrington rotation, we generate a synoptic map, updated daily though.


Routine production
Routine Production below the photosphere) flow maps and sound-speed perturbation maps for the following two types:


2 user designated area
2. User Designated Area below the photosphere) flow maps and sound-speed perturbation maps for the following two types:

Input

output

Users are free to select their interested active regions, and request a computation of cross-covariance or subsurface structures.


Flow chart for time distance pipeline
Flow Chart for Time-Distance Pipeline below the photosphere) flow maps and sound-speed perturbation maps for the following two types:


Tracking remapping and time distance measurement
Tracking, Remapping, and Time-Distance Measurement below the photosphere) flow maps and sound-speed perturbation maps for the following two types:

Each of 25 areas is tracked with the Snodgrass rate at the center of the area, and each area has a dimension of 512x512x640 with a spatial sampling of 0.06o/pixel, and a temporal cadence of 45 sec. Phase-speed filtering is then applied. After time-distance measurement, the resultant dimension becomes 256x256 with 0.12o/pixel.

annulus # phase speed (μHz/l) FWHM annulus range (deg)

1 3.40 1.00 0.54 – 0.78

2 4.00 1.00 0.78 – 1.02

3 4.90 1.25 1.08 – 1.32

4 6.592 2.149 1.44 – 1.80

5 8.342 1.351 1.92 – 2.40

6 9.288 1.173 2.40 – 2.88

7 10.822 1.895 3.12 – 3.84

8 12.792 2.046 4.08 – 4.80

9 14.852 2.075 5.04 – 6.00

10 17.002 2.223 6.24 – 7.68

11 19.133 2.03 7.68 – 9.12


Initial Results from HMI: below the photosphere) flow maps and sound-speed perturbation maps for the following two types:

Routine Production of Synoptic Maps


Power spectrum and time distance diagram
Power Spectrum and Time-Distance Diagram below the photosphere) flow maps and sound-speed perturbation maps for the following two types:


Subsurface flow field at the depth of 1-3 Mm. below the photosphere) flow maps and sound-speed perturbation maps for the following two types:


Map for divergence supergranulation
Map for Divergence (Supergranulation) below the photosphere) flow maps and sound-speed perturbation maps for the following two types:

Divergence computed from horizontal flow fields at the depth of 0-1 Mm. Positive regions represent positive divergence, i.e., supergranules.


Plenty of supergranulation
Plenty of Supergranulation! below the photosphere) flow maps and sound-speed perturbation maps for the following two types:

Every 8 hours, we have full-disk supergranulation maps at different depths. The plentiful data will be very useful for supergranulation studies.


Divergence times vorticity
Divergence times Vorticity below the photosphere) flow maps and sound-speed perturbation maps for the following two types:

Horizontal component of divergence multiplying the vertical component of vorticity represents kinetic helicity, in some sense. This value has clear latitudinal dependence, and that is mainly caused by the Coriolis force.


Synoptic flow chart large scale flows
Synoptic Flow Chart (Large Scale Flows) below the photosphere) flow maps and sound-speed perturbation maps for the following two types:

This flow chart displays large scale flows comparable to the ring-diagram analysis. The original flow map has 3000x1000 vectors, but this map only has 120x40 vectors. This rotation covers from May 19 to June 17, 2010.


Interior rotation and meridional flow speed
Interior Rotation and Meridional Flow Speed below the photosphere) flow maps and sound-speed perturbation maps for the following two types:


An Example of User Designated Area below the photosphere) flow maps and sound-speed perturbation maps for the following two types:


Flow field beneath an active region
Flow Field beneath an Active Region below the photosphere) flow maps and sound-speed perturbation maps for the following two types:


Ring-Diagram Helioseismology Analysis Pipeline below the photosphere) flow maps and sound-speed perturbation maps for the following two types:


Far-Side Active Region Imaging Pipeline below the photosphere) flow maps and sound-speed perturbation maps for the following two types:

(Largely Not Yet Ready)


Solar far side image from helioseismic holography
Solar Far-Side Image from Helioseismic Holography below the photosphere) flow maps and sound-speed perturbation maps for the following two types:

The Sun is not transparent to light, but it is completely transparent to acoustic waves. However, it is not an easy thing to image the active regions in the far-side of the Sun.

Lindsey & Braun, 2000, Science, 287, 1799

Figure courtesy: SOHO/MDI


Solar far side image from time distance
Solar Far-Side Image from Time-Distance below the photosphere) flow maps and sound-speed perturbation maps for the following two types:


To download data, go to page: below the photosphere) flow maps and sound-speed perturbation maps for the following two types:

http://jsoc.stanford.edu/ajax/lookdata.html


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