Mauna Kea Observatory infrared observations

Galactic and solar system infrared observations are reported using a broad variety of radiometric and spectroscopic instrumentation. Infrared programs and papers published during this period are listed

Astronomical studies of the major planets, natural satellites and asteroids using the 2.24 m telescope

Directional features in the Jovian sodium torus, high quality CCD images of the major planets, methane bands in the spectrum of Triton, the central wavelength of the SO2 absorption band on Io, a component on the icy surfaces of the satellites of Uranus, fluctuation of Io's volcanic radiation, standard stars, and thermal radiation from the four brightest satellites of Uranus are discussed

Temperature distribution in a stellar atmosphere diagnostic basis

A stellar chromosphere is considered a region where the temperature increases outward and where the temperature structure of the gas controls the shape of the spectral lines. It is shown that lines which have collision-dominated source sink terms, like the Ca(+) and Mg(+) H and K lines, can be used to obtain the distribution of temperature with height from observed line profiles. Intrinsic emission lines and geometrical emission lines are found in spectral regions where the continuum is depressed. In visual regions, where the continuum is not depressed, emission core in absorption lines are attributed to reflections of intrinsic emission lines

A search for N-type galaxies

A large number of distant clusters of galaxies was examined for the presence of a bright compact galaxy or blue stellar object. Nearly 600 square degrees of sky were searched using glass copies of the National Geographic Society-Palomar Observatory Sky Survey plates, and over 20 fields were selected for observation. The objects were examined for infrared and ultraviolet excesses, using wideband filter photography and spectroscopy. Initial findings include a faint, distant cluster of galaxies near the quasi-stellar radio source 4C 37.43 with a red shift of 0.370. One of these galaxies has an emission line at 6895 A, indicating a possible red shift of 0.377 of the 5007 A line of (0 III)

Research in planetary astronomy and operation of Mauna Kea Observatory

Highlights of the programs including the major planets, satellites, asteroids, and comets are presented. The operation of the 2.24 m telescope is discussed

Coronal and chromospheric physics

Achievements and completed results are discussed for investigations covering solar activity during the solar maximum mission and the solar maximum year; other studies of solar activity and variability; infrared and submillimeter photometry; solar-related atomic physics; coronal and transition region studies; prominence research; chromospheric research in quiet and active regions; solar dynamics; eclipse studies; and polarimetry and magnetic field measurements. Contributions were also made in defining the photometric filterograph instrument for the solar optical telescope, designing the combined filter spectrograph, and in expressing the scientific aims and implementation of the solar corona diagnostic mission

Submillimeter observations of solar limb-brightening in the total solar eclipse of 31 July 1981

Eight flights of the Kuiper Airborne Observatory (KAO) were devoted to solar observation. The successful observation of a total solar eclipse was accomplished. The observations were made simultaneously at 30, 50, 100, and 200 microns. The successful adaptation of the KAO for solar observations thus provided the most detailed data to date in this spectral band. The results from a preliminary analysis of the KAO data are summarized: (1) the 200 micron limb is extended about 3 arc sec above the 30 micron limb, indicating the prescence of cool dense material up to the altitudes of spicules; (2) strong radial darkening of the quiet sun intensity profile appeared at 200 microns, probably an indication that hot material in the low chromosphere is recessed into vertical magnetic flux tubes embedded in a cooler nonmagnetic substrate, which obscures the heated material approaching the limb; (3) active regions were observed to undergo a strong increase in contrast above the quiet sun background at wave lengths of 100 microns and longer; and (4) the moon was mapped for use as a photometric standard for determining the absolute intensity of the sun in all four wavelength bands

Extreme limb profiles of the sun at far-infrared and submillimeter wavelengths

Thirty, 50, 100, and 200 microns solar limb intensity profiles determined with arcsecond resolution from airborne observations of the occultation of the solar limb during the total eclipse of 1981 July 31 are presented. Two points of particular importance emerge: (1) the longer-wavelength (100 and 200 micron) limbs are significantly brighter than disk center. At 200 microns the extreme limb is about 1.22 times the brightness of disk center. This is consistent with the 6000 K temperature-plateau structure of the model chromospheres of Vernazza, Avrett, and Loeser (1973, Ap. J., 184, 605; 1981; Ap. J. Suppl., 45, 635;) and (2) the longer wavelength limbs are extended significantly further above the visible limb than Vernazza, Avrett, and Loeser predict. These results provide a strong basis for modeling of the solar chromosphere free from the assumption of gravitational-hydrostatic equilibrium

Submillimeter extensions of the solar limb determined from observations of the total eclipse of 1981 July 31

First results are presented of observations of a lunar occultation of the solar limb made from the Kuiper Airborne Observatory in the 30 micrometr, 50 micrometer, 100 micrometer, and 200 micrometer continuum during the total solar eclipse of 1981 July 31. The solar limb was extended at the longer wavelengths up to 1000 km higher than predicted from smooth plane-parallel chromospheric models. Results at both second and third contact show the infrared limb extensions to be approximately 0".8, 1"5, 2".5 and 3".0 above the visible limb in the observed bands, respectively. A possible interpretation proposes chromospheric fine structure inhomogeneities of greater density than presently incorporated in models of the middle chromosphere

Playful interactions: A critical inquiry into interactive art and play

My practice-based doctoral research explores how I, as an artist, can create conditions and possibilities for playful interaction in and around interactive artworks. Using practice- based research methods four artworks were created, presented and examined in relation to my research questions concerning play. The three key research questions were:1] How do the properties and affordances of materials and technologies foster play and interactions?2] How can artists conceptualise physical participation and play in interactive artworks? 3] What kind of play takes place in and around interactive artwork?My inquiry focused on the development of a model for making playful and interactive artworks and the creation of a vocabulary of play, which demonstrates the different kinds of play initiated through my practice and research. The model provides alternative ways to think about the role of play within interactive art and consists of a series of tangible making gambits for eliciting playful interactions from the audience. The model will be useful for future interactive artists, as well as other fields concerned with the creation of playful experiences. Underpinning my process of creating playful experiences were methods of observation of the participants’ interactions, which were used in order to enable change and improvement of the artworks throughout the research process.I argue that by employing a sculptural approach to interactive art, using the visual arts tradition of working with the properties of materials and affordances of technology, an invitation to play was created. I propose that to focus on the material’s affordance, rather than on interactive systems, provides additional ways to create interactivity. I also suggest that by understanding technology as a sculptural and embodied material we can move the focus from the technology to what the art does and says. In this sculptural playful interactivity audience members are allowed and encouraged to touch and physical and immersive participation is invited. I explored the body as a particular mode of interaction that can bridge the divide between doing and looking in the gallery, developing theories of the playful body and how audiences connect through play. I argue that the combination of sculptural, captivating interfaces, where the artwork reacts reliably, enables the audience to develop play mastery and become fully engaged. These playful interactions invite people to be curious and seek to engage audiences into dialogue, thereby opening up the possibility for play. Play is an essential pre-condition for the emergence of possibilities and, as such, it is the flexible structure by which meaningful interaction can arise. These interactions are not about our relation to technology but rather about new ways of experiencing culture. In this context interactive art is part of a wider change in contemporary art, where artists are creating culture to be experienced rather than consumed