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Deep Space Network support of the Helios mission is reported. Downlink signal degradation on the Helios-1 spacecraft and occultation of Helios-2 are discussed. Capability and performance of the network are assessed.
Deep Space Network coverage of Helios-1 and Helios-2 from Feb. 1 through Apr. 15, 1977 is presented in tabular form. Mark III data system (MDS) performance and station modifications for MDS configuration are discussed. Cross support for Helios operations by DSN and STDN is described and their downlink performances compared.
Deep Space Network support of Helios mission operations includes information on Helios-1's seventh perihelion, Helios-2's fifth perihelion, and other mission-related activities.
Deep Space Network support of Helios mission operations is discussed. Included is information on the Helios 1, 7th aphelion, Helios 2, 5th aphelion, science experiments, 22-bit error polynomial code (EPC) testing, and other mission-related activities. Mission operations and status are summarized and specific correction commands are described. Special activities and experiments include Faraday rotation data collection and a solar wind tracks experiment.
Observations of five gamma-ray bursts made with the solar orbiter Helios-2 are reported. Wavefront timing from Helios-2, at distances of up to 1.98 AU, to Vela-5A and -6A, in Earth orbit, provides source location bands as narrow as 2 arc minutes, although several degrees in length. The burst intensities and time profiles measured in interplanetary space by Helios-2 are the same as those observed near the earth, ruling out a narrow-beam interplanetary origin model. Also, the source direction bands for these events are inconsistent with the directions of all known celestial X-ray objects, X-ray bursters and high-energy gamma-ray source regions. The gamma-ray burst source objects therefore appear to form a distinct class from all lower energy X-ray or higher energy gamma ray emitters.
Observations of five gamma-ray bursts made with the solar orbiter Helios 2 are reported. Wavefront timing from Helios 2, at distances of up to 1.98 AU, to Vela 5A and 6A, in earth orbit, provides source location bands as narrow as 2 arcmin, although several degrees in length. The burst intensities and time profiles measured in interplanetary space by Helios 2 are the same as those observed near the earth, ruling out a narrow-beam interplanetary origin model. Also, the source direction bands for these events are inconsistent with the directions of all known celestial X-ray objects, X-ray bursters, and high-energy gamma-ray source regions. The gamma-ray burst source objects therefore appear to form a class distinct from all lower-energy X-ray or higher energy gamma-ray emitters.
A survey of the electron content measurements during solar occultations of the Helios A and B spacecraft is presented, and a spectral analysis using the method of maximum entropy is discussed. Typical variations measured are on the order of 0.1-1.8 x 10 to the 18th/sq m, while typical values for the rate of change are 0.7-50 x 10 to the 13th per sq m per sec. Numerical results in agreement with findings from Helios radio science, reveal a fundamental period of about 70 minutes superimposed by minor spectral peaks corresponding to shorter time periods such as 35 and 25 minutes. In addition, the periodicities observed in electron content are discussed in terms of fast hydromagnetic waves excited by nonlinear Alfven waves via coupling terms before crossing the Helios ray path. It is noted that for the first time experimental evidence is presented that hydromagnetic waves may actually be propagating from the solar corona into the interplanetary medium.
A method for displaying the electron Thomson scattering intensity in the inner heliosphere as observed by the zodiacal light photometers on board the Helios spacecraft in the form of synoptic maps is presented. The method is based on the assumption that the bulk of the scattering electrons along the line of sight is located near the point closest to the sun. Inner-heliospheric structures will generally be represented properly in these synoptic maps only if they are sufficiently long-lived (that is, a significant fraction of a solar rotation period). The examples of Helios synoptic maps discussed (from data in April 1976 and November 1978), indicate that it is possible to identify large-scale, long-lived density enhancements in the inner heliosphere. It is expected that the Helios synoptic maps will be particularly useful in the study of corotating structures (e.g., streamers), and the maps will be most reliable during periods when few transient featurs are present in the corona, i.e., during solar minimum.
We display the electron Thomson scattering intensity of the inner heliosphere as observed by the zodiacal light photometers on board the Helios spacecraft in the form of synoptic maps. The technique extrapolates the brightness information from each photometer sector near the Sun and constructs a latitude/longitude map at a given solar height. These data are unique in that they give a determination of heliospheric structures out of the ecliptic above the primary region of solar wind acceleration. The spatial extent of bright, co-rotating heliospheric structures is readily observed in the data north and south of the ecliptic plane where the Helios photometer coverage is most complete. Because the technique has been used on the complete Helios data set from 1974 to 1985, we observe the change in our synoptic maps with solar cycle. Bright structures are concentrated near the heliospheric equator at solar minimum, while at solar maximum bright structures are found at far higher heliographic latitudes. A comparison of these maps with other forms of synoptic data are shown for two available intervals.
This report is the documented result of an Internal study effort to examine possible spacecraft configurations for flight to within 0.20 AU of the sun. The objective of this study was to optimize the HELIOS spacecraft design for flights closer than 0.3 AU without jeopardizing the HELIOS Project costs or schedule. The results of the study meet this objective. In addition to this written report, an oral presentation has been prepared for the Second HELIOS Joint Working Group Meeting at GSFC on 27 April 1970. In the performance of this study, Messerschmitt-Bolkow-Blohm GMBH was assisted by the General Electric Company, Missile and Space Division, Valley Forge, Pennsylvania.
Welcome to the HELIOS Technology Challenge Guide. This document is intended to serve as a general road map for participants of the HELIOS Technology Challenge [HTC] Program and the associated inaugural challenge: HTC-01: Cost-Effective Additive Manufacturing in Space. Please note that this guide is not a rule book and is not meant to hinder the development of innovative ideas. Its primary goal is to highlight the objectives of the HTC-01 Challenge and to describe possible solution routes and pitfalls that such technology may encounter in space. Please also note that participants wishing to demonstrate any hardware developed under this program during any future HELIOS Technology Challenge showcase event(s) may be subject to event regulations to be published separately at a later date.
The Parker Solar Probe and the incoming Solar Orbiter mission will provide measurements of solar energetic particle (SEP) events at close heliocentric distances from the Sun. Up to present, the largest data set of SEP events in the inner heliosphere are the observations by the two Helios spacecraft. Aims.We re-visit a sample of 15 solar relativistic electron events measured by the Helios mission with the goal of better characterizing the injection histories of solar energetic particles and their interplanetary transport conditions at heliocentric distances <1AU. Methods. The measurements provided by the E6 instrument on board Helios provide us with the electron directional distributionsin eight di erent sectors that we use to infer the detailed evolution of the electron pitch-angle distributions. The results of a Monte Carlo interplanetary transport model, combined with a full inversion procedure, were used to fit the observed directional intensities in the 300–800 keV nominal energy channel. Unlike previous studies, we have considered both the energy and angular responses of the detector. This method allowed us to infer the electron release time profile at the source and determine the electron interplanetary transport conditions. Results. We discuss the duration of the release time profiles and the values of the radial mean free path, and compare them with thevalues reported previously in the literature using earlier approaches. Five of the events show short injection histories (<30 min) at the Sun and ten events show long-lasting (>30 min) injections. The values of mean free path range from 0.02AU to 0.27AU.Conclusions. The inferred injection histories match with the radio and soft X-ray emissions found in literature.We find no dependence of the radial mean free path on the radial distance. In addition, we find no apparent relation between the strength of interplanetary scattering and the size of the solar particle release.
An overview is presented concerning the basic NASA ground rules, guidelines, and practices associated with the establishment and conduct of a NASA international cooperative project. The Helios project is the most expensive and scientifically most significant of all of the NASA unmanned cooperative satellites considered. An agreement signed in June 1969 provided for Germany to develop a flight spacecraft with both American and German scientific instruments aboard that would be launched by the U.S. on two separate missions toward the sun. Details of the Helios mission are discussed along with aspects of spacecraft design, subsystem characteristics, and the scientific experiments.
The severe HELIOS mission environment asked for an appropriate material selection for optical surfaces based on a good approach to predict degradation and contamination effects by analysis and an adequate vertification by test. Analysis results are compared with flight data of the HELIOS-A mission.
The Helios-1 spacecraft has completed its dual superior conjunctions and second perihelion passage of the Sun and is rapidly approaching its second aphelion, near the Earth's heliocentric trajectory. Valuable scientific data were obtained during these two important events. Helios-B testing activities are proceeding according to schedule, with test results reported in this article.
Helios is the German-American solar probe which comes within 0.31 Astronomical Units of the sun. A special thermal design and a dry lubrication system have resulted in successful operation up to now, with Helios having finished its first orbit around the sun.
The Experiment 5 Antenna deployment problem onboard Helios A, the failure analysis, and changes in design, test, and operation which led to a successful deployment of both antennas during the early Helios B mission phase are described.
The successful flight of the Helios-1 spacecraft continues as it approaches its third aphelion. The Helios-2 spacecraft has entered its first superior conjunction and continues in excellent health. Much valuable scientific information about the solar corona and its effects on electromagnetic waves is expected to be learned from data gathered during this superior conjunction.