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Campaigns with HASTA data coverage
  

November 2000: MEOC CAMPAIGN (MM_OP 008)

15 Sep- 27 Oct 2000: Doppler Shifts in X-ray Jets SOHO JOP 104 

6-11 September 2000: High-cadence CME tracking SOHO JOP 127

10-27 January 2000: "ANTARTIDA": SOHO JOP 117

3-11 November 1999: Pre-Eruptive Filament Structures SOHO JOP 114

12-19 August 1999: SIGMOID CAMPAIGN MMOC002 

8-14 April 1999: The SOHO Joint Observation Program JOP 099



MEOC CAMPAIGN: Moreton/EIT Obseving Campaign

Link to the Meoc Home Page in IAFE- Buenos Aires

Scientific Goals

We intent to observe the corona before and after a CME, in order to detect a possible relation between this phenomena and the Moreton and EIT waves. With observations performed in the Ha wings, employing EIT differences images and studying radio and SXR signatures we pretend to analyze their behavior.

We also hope to receive observational contributions from other observatories interested in this subject.

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   DOPPLER SHIFTS IN X-RAYS JETS SOHO JOP 104

Objectives:

1. Obtain Doppler shifts in X-ray jets to test reconnection scenarios proposed to explain the X-ray structure.

2. To identify the origin and fate of high velocity, compact plasmoids that are seen as small regions of high Doppler shifted emission in the corona above active regions on the limb.

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HIGH-CADENCE CME TRACKING  SOHO JOP 127

The proposed programme of observations uses IPS observations from EISCAT (931 MHz, 14-100 R) and Toyakawa (327 MHz, 30-250 R), together with high-cadence optical measurements from LASCO C2 and C3, Nancay radioheliograph data, EUV imaging from TRACE, green-line imaging from MICA, H-alpha from HASTA and white-light images from the MLSO Mk.4 coronagraph and in-situ measuremets from Ulysses as it approaches its southern polar pass. Together these will provide unprecidented coverage of the corona and solar wind from the lower corona to beyond 400 R.

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MAX MILLENNIUM "ANTARTIDA": FLARE GENESIS SOHO JOP 117_ # 004

We observed together with the Flare Genesis Experiment. Observations are full disk, every 1.5 min in quiet mode and every 15 seconds in flare mode. The normal sunny hours run in this summer time from 12 to 21 UT approximately. Every hour we got some images in the wings of H-alpha. See the month-log for January, 2000.

Ask me to get the full observed time-log or the images for any day.

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 PREERUPTIVE FILAMENT STRUCTURES: SOHO JOP 114

The goal of this campaign is to observe the pre-eruptive structure and mass motions in 1 to 3 filaments and their overlying coronal arcades. This study would help in forecasting the properties of interplanetary clouds associated with CMEs and eruptive filaments, which are important with regard to Space Weather. Observing period: Nov 3-10, 1999.

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SIGMOID CAMPAIGN MMOC002 (AR 8668):

NOTE: Unfortunately, the data for these days were mostly taken with a 5 min cadence in the H-alpha line center. All the images are full disk, 1280x1024 pixels.
  Observation days for this Campaign: 14, 15, 16, 17 and 18 August 1999.

Here are some HASTA gifs images or movies:

14 August 1999: Data from 12:03 till 20:13 UT.
Get the observation hours for this day (txt).
EXAMPLES:
   
15 August 1999: No data
   
16 August 1999: Data from 11:59 till 19:56 UT.
Get the observation hours for this day (txt).
EXAMPLES:
   
17 August 1999: Data from 12:19 till 19:56 UT (data from 12:49 till 12:55 UT every 15 sec)
Get the observation hours for this day (txt).
EXAMPLES:
     
  
18 August 1999: The data are OK, but the observation time is not accurate.
 

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THE SOHO JOINT OBSERVATION PROGRAM JOP 099
It was the first official campaign for the new instruments in Argentina. It was running for the first time in April, 1999. The aim of JOP 099 is studying filaments that are likely to erupt, (e.g., long filaments, filaments lying in an AR with emerging flux, or filaments between connected ARs, etc). During this first run of JOP 099 we have obtained data from CDS on-board SOHO, TRACE and HASTA, together with synoptic data from MDI, EIT, and LASCO (SOHO), SXT (Yohkoh) and MICA. As the JOP was finished recently, the data analysis is very preliminary, but the first results could be seen in Bagalá et al. (1999b). HASTA helped before the JOP started, in choosing the adequate filament, and during the JOP with images of the evolution of the filament/prominence. During the on-limb study, they could determine the onset of CME, measuring in the wings of H-alpha.

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Last updated: September, 2000.