CCD spectroscopy of the W Serpentis binaries KX And and RX Cas

Initial results are presented from a study of H profiles in the two interacting binaries KX And and RX Cas of W Serpentis type. The used CCD spectra with a resolution of 0.13Å/px were obtained with the 2.2m telescope and the Coudé spectrograph at the German-Spanish Astronomical Center at Calar Alto/Spain.KX And. This star is probably a non-eclipsing member of the W Serpentis type interactive binaries and has a period of P = 38.908 days. Our seven spectra of KX And were obtained at phase 0.54 – 0.75. The P Cyg profiles of the H line during our observations indicate an expanding shell. The asymetry becomes blue-sided at phase 0.67 and increases thereafter. This points toward a strong outflow of matter in the vicinity of the L3 point.RX Cas. According to the model of Andersen et al. (1988) the primary is a mid-B type star with M = 5.8M and R = 2.5R . The star is completely obscured by a geometrically and optically thick disk, which is supplied by mass transfer from the other component. The secondary is a K1 giant with M = 1.8M and R = 23.5R and fills out his critical Roche lobe. Radiative and geometrical properties of the disk are variable and its structure is probably not homogenous.Five spectra of RX Cas were obtained during the primary eclipse (phase 0.95 – 0.19). The observed double-peak emission is seen only after the eclipse with a separation of 250 km/s peak-to-peak, while during the eclipse an asymetric line profile can be observed with a red-shifted emission always presented. Also, a central emission at = 0.94 should be noticed, probably originating in the vicinity of L1.The observations of both systems indicate that we are dealing with strongly interacting binaries. Further observations are planned for better covering of phase.Visiting Astronomer, German-Spanish Astronomical Center, Calar Alto, operated by the Max-Planck-Institut für Astronomie Heidelberg jointly with the Spanish National Commision for Astronomy.     

CCD spectroscopy of the W Serpentis binaries KX And and RX Cas

Initial results are presented from a study of H _γ profiles in the two interacting binaries KX And and RX Cas of W Serpentis type. The used CCD spectra with a resolution of 0.13Å/px were obtained with the 2.2m telescope and the Coudé spectrograph at the German-Spanish Astronomical Center at Calar Alto/Spain. KX And. This star is probably a non-eclipsing member of the W Serpentis type interactive binaries and has a period of P = 38.908 days. Our seven spectra of KX And were obtained at phase 0.54 – 0.75. The P Cyg profiles of the H _γ line during our observations indicate an expanding shell. The asymetry becomes blue-sided at phase 0.67 and increases thereafter. This points toward a strong outflow of matter in the vicinity of the L3 point. RX Cas. According to the model of Andersen et al. (1988) the primary is a mid-B type star with M = 5.8M _⊙ and R = 2.5R _⊙. The star is completely obscured by a geometrically and optically thick disk, which is supplied by mass transfer from the other component. The secondary is a K1 giant with M = 1.8M _⊙ and R = 23.5R _⊙ and fills out his critical Roche lobe. Radiative and geometrical properties of the disk are variable and its structure is probably not homogenous. Five spectra of RX Cas were obtained during the primary eclipse (phase 0.95 – 0.19). The observed double-peak emission is seen only after the eclipse with a separation of ≈ 250 km/s peak-to-peak, while during the eclipse an asymetric line profile can be observed with a red-shifted emission always presented. Also, a central emission at φ = 0.94 should be noticed, probably originating in the vicinity of L1. The observations of both systems indicate that we are dealing with strongly interacting binaries. Further observations are planned for better covering of phase.     

Detailed Design of a High Speed Switched Reluctance Starter/Generator for More/All Electric Aircraft

The basic concepts and advantages of more/all electric aircraft (M/AEA) are briefly addressed. The combined starter/generator (CS/G) system is introduced as a key technology to enable M/AEA. Some important performance requirements for CS/G system are obtained. Based on these requirements, a high speed switched reluctance machine (SRM) is designed to operate as a starter/generator. The entire design process is mainly divided into two stages: electromagnetic design and thermal design. In electromagnetic design stage, the electromagnetic structure and dimensions of the machine and the number of phase winding turns per pole are obtained; the topology and main technical details of the converter are briefly introduced as well. In thermal design stage, a liquid-cooling system is designed based on the thermal analysis of the machine. In the end, the performances of the designed SRM are basically verified by simulation. To get high performances, the exciting angles are optimized in two different operating modes respectively, and the optimized performances in the motoring mode are given as well.     

Launch and early operations of Herschel and Planck

On 14 May 2009 the European Space Agency launched 2 space observatories: Herschel (with a 3.5 m mirror it is the largest space telescope ever) will collect long-wavelength infrared radiation and will be the only space observatory to cover the spectral range from far-infrared to sub-millimetre wavelengths, and Planck will look back at the dawn of time, close to the Big Bang, and will examine the Cosmic Microwave Background (CMB) radiation to a sensitivity, angular resolution and frequency range never achieved before. This paper will present the Flight Dynamics, mission analysis challenges and flight results from the first 3 months of these missions.Both satellites were launched on the same Ariane 5 and travelled to the L2 Lagrange point of the sun–earth system 1.5 million km from the earth in the opposite direction of the sun. There they were injected to a quasi-halo orbit (Herschel) with the dimension of typically 750,000 km×450,000 km, and a Lissajous orbit (Planck) of 300,000 km×300,000 km.In order to reach these Lissajous orbits it is mandatory to perform large trajectory correction manoeuvres during the first days of the mission. Herschel had its main manoeuvres on the first day. Planck had to be navigated on the first day and by a mid-course correction manoeuvre, the L2 orbit insertion manoeuvre was planned on day 50. If these slots were missed, fuel penalties would rapidly increase.This posed a heavy load on the operations teams because both spacecrafts have to be thoroughly checked out and put into the correct modes of their attitude control systems during the first hours after launch.The sequence of events will be presented and explained and the orbit determination results as well as the manoeuvre planning will be emphasised.     

First results of the growing of PbTe single crystals under microgravity conditions

Two sublimation experiments with PbTe were performed at 850°C and 750°C under microgravity conditions during the “Salyut-6”-“Soyuz-31” mission in 1978. The sublimation took place on the (100)-face of a PbTe crystal. The condensate grown at 850°C shows in the upper part the formation of a pyramidal habit. The bulk consists of parallel growth colums with [100]-boundary faces. The charge carrier concentration of the electrons (N=1,5·10¹⁹ cm^?3) is higher than the homogeniety limit for 800°C should permit. This is in contrast to the result obtained on the PbTe crystal of the parallel experiment on the earth. At 750°C a laminated condensate is grown with a low growth rate. The microphotograph of the substrate shows the beginning whisker formation according to the VLS-mechanism.     

The Western Union Telegraph Company's satellite switched TDMA advanced westar system

The Advanced Westar satellite system now being planned and developed by the Western Union Telegraph Company will replace the presently operating Westar I and Westar II satellites. The Advanced Westar space segment and ground station configuration are described.     

Bone and body mass changes during space flight

Long duration space flight has shown us that humans have significant bone loss and mineral changes because they are living in microgravity. Skylab and the longer Salyut and Mir missions, are providing us useful data and allowing us to explore the mechanism involved in skeletal turnover. Bone redistribution occurs throughout space flight with bone loss predominately in the weight bearing bones of posture and locomotion. The primary health hazards which may occur during space flight induced by skeletal changes include signs and symptoms of hypercalcemia, and the risk of kidney stones and metastatic calcification. After flight lengthy recovery of bone mass and the possible increase in the risk of bone fracture should be considered. Continued research studies are being directed toward determining the mechanisms by which bone is lost in space and developing more effective countermeasures by both the US (Schneider and McDonald, 1984 and Schneider, LeBlanc & Huntoon, 1993) and Russian (Grigoriev et. al., 1989) space programs.     

Enhanced operations efficiency by using the unified synoptic system

The unified synoptic system (USS) was developed by ESA for replacing the existing Columbus display solutions and to unify the display system used on-board and on-ground. USS provides enhanced flight operations efficiency and reduced effort for product preparation, qualification and maintenance for synoptic displays. Additional to its use for Columbus it is installed at JAXA and NASA to support requirements definition and review of NASA generated ISS displays. Due to its advanced capabilities, which go beyond existing known solutions, it has been made available to be reused for future spacecraft EGSEs and control centres (e.g. exploration missions, satellites) as well. Use of synoptic display is mostly guided by operational procedures which are in electronic format. However, till now the full operational benefit has not yet been realized. Procedure viewers and synoptic display systems are completely separate entities. Direct interaction of procedure viewers with synoptic display systems or underlying system control software is not supported at all. Therefore astronauts, flight controllers and operators still have to carry out a lot of mundane activities when executing operational procedures. The USS based procedural display viewer provides the user with a coherent, task oriented user interface for using synoptic displays and executing procedures in an efficient manner.     

Cosac, The Cometary Sampling and Composition Experiment on Philae

Comets are thought to preserve the most pristine material currently present in the solar system, as they are formed by agglomeration of dust particles in the solar nebula, far from the Sun, and their interiors have remained cold. By approaching the Sun, volatile components and dust particles are released forming the cometary coma. During the phase of Heavy Bombardment, 3.8--4 billion years ago, cometary matter was delivered to the Early Earth. Precise knowledge on the physico-chemical composition of comets is crucial to understand the formation of the Solar System, the evolution of Earth and particularly the starting conditions for the origin of life on Earth. Here, we report on the COSAC instrument, part of the ESA cometary mission Rosetta, which is designed to characterize, identify, and quantify volatile cometary compounds, including larger organic molecules, by in situ measurements of surface and subsurface cometary samples. The technical concept of a multi-column enantio-selective gas chromatograph (GC) coupled to a linear reflectron time-of-flight mass-spectrometer instrument is presented together with its realisation under the scientific guidance of the Max-Planck-Institute for Solar System Research in Katlenburg-Lindau, Germany. The instrument's technical data are given; first measurements making use of standard samples are presented. The cometary science community is looking forward to receive fascinating data from COSAC cometary in situ measurements in 2014.