How is it organized, and who will participate?. What are the goals and objectives?. What are the goals and objectives?. What is the IHY, and why now?. Q. How do you plan an activity involving 1000’s of scientists and more than 70 nations?.
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the goals and
the goals and
the IHY, and
Q. How do you plan an activity involving 1000’s of scientists and more than 70 nations?
A. Advance planning, technology, and lots of hard work
… but we have history on our side
1. IHY Secretariat
2. Regional Organizers
3. National Organizers
2. Institutes and Scientific Orgs
2. “IGY Gold” Historical Initiative
3. Education/ Public Outreach
Sponsored and Hosted by the American Geophysical Union, the IHY Secretariat includes:
1. Our new website location: ihy2007.org
2. Contact point, with IHY letterhead and official correspondence
3. Co-sponsored activities with other AGU committees and sections
4. A home for the “IGY Gold” program, co-sponsored by IUGG
Executive Director: Joseph M. Davila International Coordinator: Nat Gopalswamy
Director of Operations: Barbara J. Thompson Press Secretary: Steve Maran
IGY History Committee: Ron Doel, chair Data Systems & Analysis Committee
Publications: Rudolph Von Steiger, chair E/PO Advisory Committee
Campaign Coordination Committee
Developing Nations & Instrument Development Committee
Currently the IHY website is located at ihy.gsfc.nasa.gov
We will be migrating over to the ihy2007.org site in the next few months.
Presented to International
J. Davila (US),
R. Jain (India),
I. Veselovsky (FSU)
J.-L. Bougeret (France)
Geographic Area or Region
IHY Organizing Teams (International, National, Working Groups)
Instruments and Observatories
Scientific Interests and Disciplines
Scientific Meetings and Events
The year 2007 will be during solar minimum, approaching the rise phase of the solar cycle. This period is optimal because:
The science goals of the IHY are broad and require the coordinated effort of observatories and scientists worldwide. The scientific success of IHY requires the encouragement of innovative research programs. However, the support of a large number of these programs can strain existing resources.
Step 1. A potential campaign must be proposed through at least one campaign leader, who will serve as the chief coordinator and contact.
Step 1. A Science Working Group (SWG) identifies the need for a campaign and recruits. a campaign leader, who will serve as the chief coordinator and contact.
Step 2. The campaign proposal includes the science objectives, lists potential participating observatories and scientists, and provides an explicit description of the required observations and resources.
Step 3. The SWGs work with the Observatory Reps to determine the feasibility of the proposed observations and the scientific merit. When applicable, the Scientific Institution, Professional Organization reps and/or Emerging Nations Programs give input regarding campaign participation.
Step 4. , the SWGs place the campaign on the IHY schedule, assisting the responsible Observatory Reps in executing the campaign observations (such as target coordination).
Step 5. The Science Working Groups assist in the analysis and broaden the scientific impact of these campaigns by stimulating research, discussions, and activities at meetings.
Step 1. Dr. Almira Glover proposes a campaign to study which eruptions on the Sun produce magnetic clouds at Earth.
Step 2. Dr. Glover and her collaborators produce an IHY campaign proposal:
Title: Solar Eruptions Producing Magnetic Clouds at Earth and at 1 AU
Brief Objective: Perform a study of the magnetic structure of solar erupting regions and the associated CME structure associated with magnetic clouds at 1 AU. Include characteristics of erupting region, CME properties, possible propagation effects in the solar wind, to determine which aspects of the solar eruption can be used to predict cloud properties such as total flux, helicity, orientation, speed, and density.
Method: Examine in situ magnetic field, density, and solar wind velocity data for magnetic clouds. Obtain total flux, helicity, orientation, speed and density of cloud. Based on arrival time and speed of magnetic cloud, use a simple propagation model to determine source eruption time. Obtain solar magnetic field, H alpha, EUV, Soft X-ray and coronagraph data to obtain properties of eruption and erupting region.
Observations Required: BBSO, Wilson and MDI Magnetograms (hourly), GOES SXI images (as often as available), synoptic H alpha observations, STEREO EUVI and Coronagraph images (twice hourly), ACE solar wind observations
Campaign Duration: 2 months should produce at least 10 candidate events.
Step 3. The "Sun-Earth Transients" SWG (for example, the working groups haven’t been defined yet) forwards the proposal to the Observatory Representatives for BBSO, Wilson, MDI, GOES SXI, STEREO, and ACE SWEPAM, SWICS and MAG.
Although only synoptic observations were requested, the SWG notes that the Meudon Observatory may be available to conduct a special high-cadence H-alpha campaign, and forwards the proposal to the Meudon Observatory Representative as well.
The SWG also notes that another campaign to study the propagation characteristics of CMEs using a more intricate yet realistic model is also proposed. If possible, the SWG decides to run these campaigns concurrently so both objectives can enhance each other.
Dr. Glover's proposal is reviewed, and it is approved by all of the observers except the STEREO Coronagraph Observatory Representative, who explains that observations will only be available hourly. The proposal is accepted contingent on the agreement that the research objective is still feasible with coronagraph observations at a decreased cadence.
Step 4. Dr. Glover's campaign is approved, and it is placed on the schedule to run daily from 14 July through 22 September. Other observatories are invited to participate if interested. A daily target is chosen by a modeler on Webb's team, and the target is forwarded to the participating observatories and posted on the IHY Campaign website. The observation data is catalogued via the IHY virtual campaign database, and is thereafter accessible to IHY researchers and the public.
Step 5. The "Sun-Earth Transients" SWG assists in identifying researchers who may assist in the production of scientific results. They contact the campaign leader for the solar eruption propagation campaign and suggest that they work with Dr. Glover's team. They also identify a solar magnetic field model which includes non-potential effects, and suggest that Glover's team might benefit from using the model.
The IHY Campaign site contains all of the logistics for IHY campaign planning. It includes:
WIND MAG can only work at a 5-minute cadence (KRN)
ACE MAG has sufficient cadenceThe IHY Campaign Planning Wiki
Big Bear Solar Observatory
Bruny Island Radio Spectrometer (BIRS)
Oct 2007 Nov 2007
SAIC 3-D Solar Wind
The IHY Science Planning Database is a resource which allows IHY researchers and participants to identify scientists and observatories for campaign coordination. Because every observatory must have at least one responsible scientist, the records are indexed by participants. Searchable fields include:
The IHY Science Planning DatabaseRegister now!!At the “IHY Science” Section of ihy.gsfc.nasa.gov
The IHY Campaign Database will allow IHY researchers to easily identify and access IHY campaign data. Searchable fields will include:
All campaign planning will be migrated to a Wiki-based planning site integrated with the Science Coordination Database and Events Calendar.
Vladimir Kuznetsov, Russian Academy of Sciences, Izmiran
A great deal of the IGY’s success was due to the participation and dedication of a large community of Russian scientists. The IHY Russian planning activity is fully underway, and there are a number of Russian scientists and observatory prepared for participation in IHY. This includes the CORONAS-I, CORONAS-F and CORONAS-PHOTON missions, ground-based magnetometers, a spectromagnetograph, ionospheric monitors and an array of solar and galactic cosmic ray sites.
Cosmic Ray and Neutron Flux Monitors for IHY at the Aragats Space Environmental Center
Ashot Chilingarian, Aragats Space Environmental Center (ASEC) of the Cosmic Ray Division (CRD) of Alikhanian Physics Institute, Armenia
The ASEC consists of two high-altitude stations on Mt. Aragats in Armenia. Geographic coordinates: 40˚30′N, 44˚10′E. Cutoff rigidity: 7.6 GV, altitude 3200m and 2000 m a.s.l. At these stations, several monitors continuously measure the intensity of the secondary Cosmic Ray (CR) fluxes and send data to the Internet in real time (http://crdlx5.yerphi.am). The specifications of the ASEC monitors are shown in Table. A flexible 32-bit microcontroller-based Data Acquisition (DAQ) electronics is designed to support the combined neutron–muon detector system and utilize the correlated information from cosmic ray secondary fluxes, including environmental parameters (temperature, pressure and magnetic field). Microcontroller-based DAQ systems and high precision time synchronization of the remote installations via Global Positioning System (GPS) receivers are crucial ingredients of the new facilities on Mt. Aragats in Armenia. Main advantage of ASEC comparing with other CR monitoring centers is the multivariate, multidetector measurements of as many components of the changing secondary CR as possible. A sudden correlated variation in the flux of neutrons, muons, and electrons, detected by the surface monitors could be an indication of an upcoming severe radiation and geomagnetic storms.
IHY needs you, and we have opportunities for participants at any level of commitment. Email us at ihy@ ihy.gsfc.nasa.gov for more information!