If we could find the appropriate A and γ, then we could compute the following integral flux for any passband:

 

 

How does one determine A and γ?  This can only be done if we bring in additional information from adjacent passbands for one of the two energy channels. For example, say we wish to adjust the E3 passband to fit the upper and lower limits of the DE3 passband. One way of doing this is to model the differential count rates for E2 and E3, and assume that they both have approximately the same constant A and energy spectrum γ.  This is not a bad approximation provided the passband of E2 and E3 are adjacent to one another.  Under this assumption, we can write the following:

 

 

Taking the ratio, we see that

 

 

For EE2 and EE3 we can use the geometric mean for those particular passbands, i.e.

 

 

A little arithmetic will show that

 

 

 

Next Page

 

Updated 8/8/19, Cameron Crane

Manufacturer: ESA provided the Ulysses spacecraft, NASA provided the power supply, and various others provided its instruments.

Mission End Date: June 30, 2009

Destination: The inner heliosphere of the sun away from the ecliptic plane

Orbit:  Elliptical orbit transversing the polar regions of the sun outside of the ecliptic plane

• Ulysses Information at the Jet Propulsion Laboratory
• Ulysses Website at the European Space Agency