Several general notes on sensors used in the energetic particle studies performed by TASPD SINP MSU on non-geocentric spacecraft are given below. Many heliospheric measurements were made by TASPD SINP MSU with use of sensors that may respond to energetic particles of various species. With respect to pure measurement of some particular species, simultaneous registration of other species is considered as contamination. In some experiments, special methods against contamination were used, although in many projects none of that methods were implemented. This reflects approaches of PIs at TASPD, typical for that time. A basic principle was to measure rather global effects first, and in most cases, contamination played only insignificant role in the such-way formulated task. One reason of such position regarding pure measurements is the limitations existed that time: on capabilities of the electronic components, on the payload characteristics, on data volumes and telemetry bandwidth, etc. Another reason is a somewhat biasing of that works to the radiation safety task for which, in general, it is not necessary to perform detailed studies. And, at last, a ratio of intensities of the main species and the contaminating one was always taken into account and assumed to be large enough, in general. Among the types of sensors used at TASPD SINP MSU, only a gas-discharge counter (Geiger counter) and a silicon sensor (named below SSD - solid-state device) are concerned here. Gas-discharge counter Gas-discharge counter came to space studies from the physics of cosmic rays. It was very popular at TASPD SINP MSU due to its simplicity and reliability. A counter of the used STS-5 and, lately, SBM-20 series is a pen-like tube of ~9 cm length and ~1 cm diameter. That sensor counts particles arriving from approximately all directions. Protons and electrons may be registered with almost 100% efficiency. Gas-discharge counter has been used in almost all instruments by TASPD for non-geocentric spacecraft. Specifications of installation are, in general, the same for every mission: typically, the counter is mounted on a side of a spacecraft under the shielding of about 1 g/cm2 Al. It corresponds to ~30 MeV energy threshold for protons and ~1 MeV - for electrons. A view angle with such shielding conditions is assumed to provide a geometric factor ~13 cm2_sr. In other directions a sensor is shielded with the spacecraft body that assumed to correspond to ~500 MeV energy threshold for protons. Such energetic particles may arrive to the counter from all directions; the geometric factor for them is ~54 cm2_sr. Identification of data from gas-discharge counter measuring in interplanetary space is based on the properties of the particle fluxes there. Falling form of a power spectrum of protons allows one to neglect the >500 MeV component in most cases. Electrons of Ee>1 MeV from solar flares typically arrive to a sensor before protons of Ep>30 MeV, and flux of protons from a flare typically lasts much longer than the electron flux from the same origin. Hence, the following results from a gas-discharge counter may be considered as the rather reliable: a background level of galactic-originated protons of Ep>30 MeV and its long-term variations; a general shape of solar-flare-originated protons of Ep>30 MeV (not in the beginning part of an enhancement). A windowed discharge counter of SBT-9 series was widely used too. It looks like SBM-20 but about twice shorter and it has a window of mica at his butt-end. This window has square size of ~0.2 cm2 and it allows one to register protons with Ep>0.8 MeV and electrons of Ee>40 keV and gamma-quanta of Eg>4 keV. Information on solar gamma-bursts may be easily identified in the data of solar-directed windowed counter due to short duration of such bursts. Also, the data from a similar counter that does not directed to sun may be used for separation of gamma-quanta. Involving of the data from a counter without window may help in separation of low-energy particles measured with window from the higher energy component measured through the counter's body. Silicon sensor Sensors of SSD type were widely used in instruments made at TASPD SINP MSU. In many simple monitors of charged particles, a stand-alone SSD has been used. Such simple technique is subject to contamination by several ways. These ways and their effect on the measurement results are briefly discussed below. Stand-alone SSD sensor is a plate of Si covered by thin foil and placed under a collimator with a hole of the cone form. Geometric factor for such instrument may be derived from the size of the open part of a Si plate and the solid angle of a collimator. Energy channels of the sensor depend on the thickness of the used foil, and on the thickness of the Si plate, and on the chosen thresholds of a pulse-amplitude analyser. Regarding normal measuring of the proton flux, contamination may appear in the following ways: 1. electrons arriving to sensor via the aperture cone; 2. protons of higher energy from outside the aperture (across collimator walls); 3. electrons of high energy from outside the aperture (across collimator walls); 4. overlapping of pulses from high-intensity flux of low-energy particles. An efficiency of registration of an electron depends on its energy, thickness of a SSD and the lower threshold of an energy channel. In most cases, aluminum foil of ~0.01 mm thickness is used for covering a SSD sensor. In such foil proton loses 300-500 keV while electron crosses it without notable losses. Electrons are almost not registered in SSD if its thickness is less than 0.3 mm. If SSD's thickness is around 1-1.5 mm, an efficiency is as large as 0.8-0.9 for electrons with energy just above a threshold, but it decreases with electron energy as steeply as one order of magnitude per one MeV. For SSD thicker than 2 mm, the efficiency equal to 0.8-0.9 and it does not depend on energy of electron. For energy channels with threshold for protons Ep>4 MeV, electron contamination becomes practically negligible since electrons cannot leave so much energy in the SSD of used thickness. For a typical case, thickness of collimator walls may be estimated as ~1.5 g/cm2 Al. Electron loses ~3 MeV penetrating such a wall. Arrival of particles crossing the collimator's wall must be considered with other geometric factor than the arrival via aperture. If normal geometric factor G0 is calculated for aperture cone of +-30 degrees, the geometric factor G1 for arrival of electrons crossing a wall is about 3*G0. If the cone angle is +-25 degrees, as is on GRANAT, G1=~5*G0. Penetrating a wall of 1.5 g/cm2 Al, proton loses about 35 MeV so that it must have energy Ep>35 MeV to be measured in the energy channel Ep>1 MeV. For the energy channel Ep>10 MeV original proton energy must be Ep>45 MeV. To estimate contamination of a proton channel by protons arriving from outside the aperture, a power spectrum of the proton flux with the power index A=2 could be considered. In this case, additional protons contribute as much as ~0.5% into the 1 mm SSD in the energy channel Ep>1 MeV and ~40% in its channel with Ep>10 MeV. In practice, overlapping of pulses from the high-intensity flux of low-energy particles may be realized in the Earth's radiation belts. This is seen in the data from a thick SSD on GRANAT: electrons of Ee>350 keV are measured in the channel for protons of Ep>1.2 MeV and electrons of Ee>2.3 MeV are measured in the channel for protons of Ep>5.1 MeV. In the case of Ep>1.2 MeV, for example, two coincided pulses from ~350 keV electron each give in sum a pulse that reaches a level of 700 keV. However 700 keV just corresponds to the proton energy Ep=1.2 MeV since a proton loses about 500 keV in the foil on arrival. The mentioned energies of electrons Ee>350 keV and Ee>2.3 MeV must be understood as somewhat mean values since 700 keV, for example, may be resulted with combinations either 350 keV + 350 keV or 300 keV + 400 keV etc. The described effect of overlapping was not expected as realizable since the instrument KS-18-M has not been designed for working in radiation belts at all.