Heliosphere: Cassini/INCA and Voyager measurements entail no tail

The INCA detector on Cassini has been measuring 5.2-55 keV Energetic Neutral Atoms from the heliosphere since 2003, while the LECP instruments on Voyager-1 (>40 keV) and Voyager-2 (>28 keV) have been taking in-situ ion measurements from the heliosheath (HS) after crossing the termination shock (TS), 35deg north (2004) and 32deg south (2007) of the ecliptic plane at 94 and 84 AU, respectively. The comparison between in-situ ions and remote sensed ENAs in overlapping energy bands has led to several key discoveries concerning the heliosphere interactions with the LISM. Some of those are summarized as follows: (A) The "Belt", identified as a high intensity and wide ENA region that encircles the celestial sphere in ecliptic coordinates corresponds to a "reservoir" of particles that exist within the heliosheath and the "Basins", identified as two extended heliosphere lobes where the ENA minima occur; both constantly replenished by new particles from the solar wind; (B) The interstellar magnetic field was estimated to be 0.5 nT (<0.64 nT), stronger than was assumed before in order to balance the nonthermal pickup ion pressure in the heliosheath, which was confirmed a few years later, after V1 crossed the heliopause; (C) The V1 crossing of the heliopause per se was predicted within a month, implying a heliosheath thickness of LV1 27(+26, -11) AU, whereas recent analyses of our measurements imply that the thickness along the V2 line-of-sight might be twice as thick; (D) Strong intensity/pressure gradients in the anti-nose ENA measurements (tail to basin drop rate of 2.4% per degree), taken together with the fact that the pick-up ion populations, in keV range play dominant role in maintaining the pressure balance in the heliosheath, pointed to the "diamagnetic" character of the heliosheath; (E) The heliosphere forms a time-dependent roughly symmetric obstacle to the inward interstellar flow, responding within 2-3 yrs, in both the nose and anti-nose directions to the outward propagating changes of the solar wind throughout the solar cycle. These results, taken together with the V1 measurements of Bismf 0.5 nT, nH>0.1/cm3, and increased plasma beta inside the HS, preclude the formation of a strong bowshock, and strongly suggest a diamagnetic bubble-like heliosphere with few substantial tail-like features.