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The Swedish Institute of Space Physics is developing a miniature plasma analyzer for planetary missions (MIPA—Miniature ion precipitation analyzer). MIPA has been accepted to fly on-board both the ESA BepiColombo mission to Mercury (2014) and the Indian Chandrayaan—1 mission to the Moon (2007). The analyzer measures ions in the energy range 10 eV–15 keV and has a sufficient mass resolution to resolve the main groups of ions, namely

M / q = 1, 2, 4, 8, 16, > 30

. Field of view is

9^{\circ} \times 180^{\circ}

. The instrument consists of the sensor head and a separate electronic board whose total mass is 300 g. The sensor head envelope is roughly

53 \times 85 \times 30 {mm}^{3}

in volume and is designed for the extreme operation temperature range of

- 100

to

+ 125^{\circ} C

. MIPA comprises an electrostatic scanner for angular resolution, a cylindrical electrostatic analyzer for energy discrimination and a time-of-flight (TOF) section for particle velocity measurement. Generic design allows using the instrument on various platforms including nano-satellite and multi-spacecraft missions. This document describes the design of the sensor part including ion optical as well as mechanical aspects. 相似文献

7.

Venus–solar wind interaction: Asymmetries and the escape of O+ ions

《Planetary and Space Science》2006,54(13-14):1472-1481

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8.

New photometric studies of two contact binaries CE Leo and V366 Cas with possible tertiary companions

《New Astronomy》2013

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9.

Limiting superluminal electron and neutrino velocities using the 2010 Crab Nebula flare and the IceCube PeV neutrino events

《Astroparticle Physics》2014

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10.

Cross section and astrophysical S-factor for 12C(p,γ)13N* reaction with Halo Effective Field Theory at low-energies

《New Astronomy》2017

We considered one of the proton halo nuclei candidates, ¹³N* nucleus, and calculated the cross section and astrophysical S-factor for ¹²C(p, γ)¹³N* reaction using halo effective field theory without pion (hEFT

^{\neg π}

). The halo effective field theory is used to examine the halo nucleus bound state with a large S-wave scattering length. We calculated the radiative proton capture cross section and the astrophysical S-factor from the fields of the core and the valence proton at the Leading-Order (LO). We showed that there is a good agreement among the our results for cross section and astrophysical S-factor of the ¹²C(p, γ)¹³N* reaction and the experimental data. The astrophysical S-factor that has been estimated at the zero energy (E_cm=0) by using a theoretical calculation of the cross section for direct radiative capture and an extrapolation of this calculation obtained

S (0) = 1.883 \times 10^{- 3}

MeV-b. 相似文献

11.

Constraints on the tidal dissipation factor of a main sequence star: The case of OGLE-TR-56b

《Planetary and Space Science》2007,55(5):643-650

The planet OGLE-TR-56b is the extrasolar giant planet closest to its host star. This planet and its star exchange extreme tidal forces. This leads to a reduction of the planetary orbit and a spin-up of the stellar rotation. The tidal migration rate depends crucially on the ratio of the tidal dissipation factor

Q_{*}

and the stellar love number

k_{2,^{*}}

of the star, which is only poorly known and estimates range within

5 \times 1 0^{5} < (Q_{*} / k_{2^{*}}) < 1 0^{10}

. For values greater than

Q_{*} / k_{2^{*}} > 1.5 \times 1 0^{9}

no observable influence by tidal forces on the planet's orbit within the lifetime for the star can be found. A lower limit for the possible values of the parameter

Q_{*} / k_{2^{*}}

for the G-type star OGLE-TR-56 was found by studying the evolution of possible tidal interaction into the future and in the past. This study demonstrates that on the basis of conservative model assumptions, a considerable but unrealistic spin-up of the star can be expected if

Q_{*} / k_{2^{*}} < 2 \times 1 0^{7}

, which is not in agreement with observed stellar rotation periods. From a statistical analysis based on a Monte-Carlo tidal evolution simulation, the