Global Model of Whistler Mode Chorus in the Near‐Equatorial Region (|λm|<  18°)

We extend our database of whistler mode chorus, based on data from seven satellites, by including ∼3 years of data from Radiation Belt Storm Probes (RBSP)‐A and RBSP‐B and an additional ∼6 years of data from Time History of Events and Macroscale Interactions during Substorms (THEMIS)‐A, THEMIS‐D, and THEMIS‐E. The new database allows us to probe the near‐equatorial region in detail, revealing new features. In the equatorial source region, |λm|<6°, strong wave power is most extensive in the 0.1–0.4fcebands in the region 21–11 magnetic local time (MLT) from the plasmapause out to L∗= 8 and beyond, especially near dawn. At higher frequencies, in the 0.4–0.6fcefrequency bands, strong wave power is more tightly confined, typically being restricted to the postmidnight sector in the region 4<L∗<6. The global distribution of strong chorus wave power changes dramatically with increasing magnetic latitude, with strong chorus waves in the region 12<|λm|<18° predominantly observed at frequencies below 0.3fcein the prenoon sector, in the region 5<L∗<8. Our extended database of whistler mode chorus allows us to probe the near‐equatorial region in great detail, revealing new featuresIn the equatorial generation region strong chorus is most extensive in the 0.1–0.4fcebands in the region 21–11 MLT from L* = 4–8 and beyondAt higher latitudes (12 <|λm| < 18°) strong chorus is largely restricted to the 0.1–0.3fcebands in the prenoon sector, from L* = 6 to 8