Tesi sul tema "Planetary bodies"
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1
Romeo, Michael Joseph. "Routing Among Planetary Bodies". Kent State University / OhioLINK, 2018. http://rave.ohiolink.edu/etdc/view?acc_num=kent1528470515838277.
2
Chabot, Nancy Lynne. "Geochemical studies of the cores of terrestrial planetary bodies". Diss., The University of Arizona, 1999. http://hdl.handle.net/10150/289052.
Abstract (sommario):
From the Earth to asteroids, numerous rocky bodies in our solar system are believed to have a metallic core at their center. However, due to the inaccessibility of these cores, fundamental issues, such as the composition of the cores or the processes of core formation and core evolution, are not well known. I have conducted both theoretical and experimental geochemical studies which have improved our understanding of the cores of terrestrial planetary bodies. The radioactive decay of K is an important planetary heat source, but the distribution of K in terrestrial planetary bodies has been debated. My experimental work, which examined the solubility of K in metal, shows no evidence for K to be an important heat source in metallic cores. The element pairs of Ag, Pd and Re, Os have been used to date core formation and core evolution events in our solar system. My experimental determination of the partitioning behavior of these important elements can be used to better understand their distribution in iron meteorites, our only samples of planetary cores. Simple fractional crystallization of a metallic core cannot explain the elemental trends observed within iron meteorite groups. I have developed a crystallization model which suggests slight inhomogeneities and mixing in the molten core were important during core evolution. As a metallic core crystallizes, liquid immiscibility may be encountered, which could significantly affect the subsequent evolution of the core. My experimental work suggests the role of liquid immiscibility during the crystallization of a metallic core is significantly smaller than the published phase diagram implies. These four topics, though each an independent project, together provide insight into the nature of the cores of terrestrial planetary bodies and the processes which affect those cores.
3
Harri, Ari-Matti. "In situ obreviations of the atmospheres of terrestrial planetary bodies /". Helsinki : Finn. Meteorological Inst, 2005. http://www.gbv.de/dms/goettingen/509702546.pdf.
4
Hilbert, Bryan (Bryan Nathaniel) 1977. "Stellar occultation lightcurve modeling for elliptical occulting bodies". Thesis, Massachusetts Institute of Technology, 2001. http://hdl.handle.net/1721.1/54444.
Abstract (sommario):
Thesis (S.M.)--Massachusetts Institute of Technology, Dept. of Earth, Atmospheric, and Planetary Sciences, 2001.Includes bibliographical references (leaf 41).
We present a new method of calculating model lightcurves for stellar occultations by the Jovian planets. We model the occulting planet as a three-dimensional body of non-zero ellipticity, and define two ellipses of intersection with the body which dictate the appearance of the lightcurve. These include the visible-limb plane ellipse, which is the observed figure of the body as seen in the sky, and the line-of-sight ellipse, which contains the line of sight to the occulted star, and is the plane in which the starlight is refracted. The observed stellar flux during the occultation is primarily dictated by the ellipticity and subsequent radius of curvature of the instantaneous ellipse in the line-of-sight plane. This new method is applied to several test cases, as well as to the Jovian occultation of HIP9369 on 10 October 1999. Lightcurves generated by this model are compared to identical situations using the method published in Hubbard et al. (1997), showing that the Hubbard model works well for low-latitude occultations, but fails at higher latitudes. In the case of the high-latitude Jovian occultation, the best-fit lightcurve, produced from this new method, yielded a half-light equatorial radius of 71,343±1.2 km with a scale height of 19.25±0.5km, and an isothermal temperature of 139K. The same data, fit using a lightcurve generated by the method described in Hubbard et al. (1997), resulted in a half-light equatorial radius of 71,819km with a scale height of 17.9km with errors comparable to the previous fit, resulting in an isothermal temperature of 129K. Lightcurves are numerically generated for an ellipsoidal planet and, for comparison, an approximation to the ellipsoidal case consisting of a sphere with radius equal to the radius of curvature of the ellipsoid at the half-light point. We find that in the case of an occultation where the line-of-sight ellipticity does not vary, that the radius of curvature approximation matches the ellipsoidal planet lightcurve to within 0.007%. For an oblique occultation however, the line-of-sight ellipticity varies, and the approximation, using only a single radius of curvature sphere, is only good to about 1%. As a result, we find that using a model such as that presented in Baum and Code (1953) to fit the lightcurve of an ellipsoidal planet can return values for half-light radius (after accounting for the distance between the center of curvature and the center of the body) which may match the local distance to the center of the ellipsoid to a fraction of a percent, while returning values of scale height which may be in error by several percent. Test cases are also then put through numerical inversions, to obtain temperature versus pressure profiles. Test cases with spherical planets return temperature profiles that match those used to create the lightcurves, while test cases with ellipsoidal planets return temperature profiles which can differ from the input temperatures by tens of degrees, assuming a constant local gravity over the course of the occultation.
by Bryan Hilbert.
S.M.
5
Theis, Karen Julia. "Iron isotope fractionation of planetary bodies during early solar system formation processes". Thesis, University of Manchester, 2008. http://www.manchester.ac.uk/escholar/uk-ac-man-scw:163898.
Abstract (sommario):
The aims of this research programme were twofold: to analyse the iron isotope compositions of metal grains from ordinary chondrite meteorites over a range of class and petrographic type to investigate redox reactions and thermal metamorphism during primitive planetesimal formation; and to analyse the iron isotope composition of secondary carbonate minerals in Martian meteorite ALH84001 to determine the formation temperature and thus constrain near surface conditions on early Mars. To analyse the iron isotope compositions of these materials it was necessary to develop a methodology using a Nu Plasma multi collector inductively coupled plasma mass spectrometer and a new technique for analysing natural iron-bearing samples without first purifying them by anion exchange chromatography. The purification process can cause fractionation within the sample which may mask small natural fractionation variations. The new methodology developed here yielded reproducible iron isotope ratios to within o.osroo (20) ensuring that small isotopic variations of (i56Fe -0.06roo to 0.3sroo were resolved during the analysis of the ordinary chondrite metal grains. The method for analysing samples containing matrix elements was successful and achieved an accuracy and precision comparable to pure analyte solutions for the analysis of the Martian carbonates. The analysis of the metal grains revealed a correlation between their iron isotope compositions and the redox and thermal metamorphism that these materials have experienced. The results indicate that the degree of iron isotope fractionation can be related to thermal metamorphism temperatures, except for metal grains from type 3 chondrites. This was interpreted as resulting from the type 3 chondrites not getting hot enough during thermal metamorphism to overprint the original igneous isotopic signatures. The a-rich carbonates in ALH84001 were petrographically characterised to place them within the known carbonate assemblage sequence which implied that the zoned carbonate deposition occurred during multiple phases. The zoned carbonates were then analysed for iron isotope composition and an isotopic fractionation variation for (i56Fe of -0.6%0 was determined relative to bulk Martian silicates. This indicated a formation temperature of approximately ±800( (20) and implied that liquid water was stable on or near the surface during this time.
6
Kanata, Sayaka. "Research on Localization and Guidance for Space Rovers on Small Planetary Bodies". 京都大学 (Kyoto University), 2010. http://hdl.handle.net/2433/123338.
7
Ruprecht, Jessica Dawn. "Astronomical studies of solar system bodies 2060 Chiron and 1 Ceres". Thesis, Massachusetts Institute of Technology, 2013. http://hdl.handle.net/1721.1/82301.
Abstract (sommario):
Thesis (S.M.)--Massachusetts Institute of Technology, Dept. of Earth, Atmospheric, and Planetary Sciences, 2013.Cataloged from PDF version of thesis.
Includes bibliographical references (p. 43-45).
In this thesis two separate projects are investigated, a stellar occultation by 2060 Chiron and rotationally resolved spectra of 1 Ceres. On 29 November 2011 UT, 2060 Chiron occulted a 14-mag star; data were successfully obtained at the 3-m IRTF on Mauna Kea and 2-m Faulkes North Telescope at Haleakala. The IRTF lightcurve shows a solid-body detection of Chiron's nucleus with a chord lasting 16.04 seconds, corresponding to a chord length of 158±14 km. Symmetric, dual extinction features in the Faulkes light curve indicate the presence of optically thick material roughly 300 km from the body midpoint. The duration of the features indicates a ~ 3 km feature separated by 10-14 km from a second - 7 km feature. The symmetry, optical thickness, and narrow size of these features allows for the intriguing possibility of a near-circular arc or shell of material. Rotationally resolved spectra of Ceres in the 0.43-0.85 micron range were observed using the DeVeny spectrograph on the Perkins 72-inch telescope at Lowell Observatory. Spectral differences as a function of phase were investigated. It is concluded that Ceres' surface is uniform at the 1% level at visible wavelengths. Additionally, the 0.6 and 0.67 pm features reported by Vilas and McFadden [1992] and Fornasier et al. [1999] are not seen at any phase at the 1% level.
by Jessica Dawn Ruprecht.
S.M.
8
Bryson, James Francis Joseph. "The origin of ancient magnetic activity on small planetary bodies : a nanopaleomagnetic study". Thesis, University of Cambridge, 2015. https://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.708801.
9
Bettella, Alberto. "Generation and propagation of vibrations on satellite structures and planetary bodies after hypervelocity impacts". Doctoral thesis, Università degli studi di Padova, 2008. http://hdl.handle.net/11577/3425965.
Abstract (sommario):
Hyper-Velocity-Impacts (HVI) are a common problem in the space environment. They especially concern space missions, in terms of:
Potential damage to spacecrafts and satellites Collisional evolution of small and large bodies of the Solar System.
This thesis focuses on the effect of such impacts, through the analysis of the vibration field generated by HVI on both of the aforementioned cases.
Referring to the first point, i.e. the HVI-induced disturbances on spacecraft internal components, a wide experimental campaign has been performed on targets representative of S/C structures, making it possible to measuring and reproducing the HVI-induced vibration field on the selected targets. The aim of this activity was to acquire data on transient waves generated after an HVI and propagating from the impact point. Such disturbances have been evaluated in from of acceleration signals.
The invaluable information achievable from such an activity is related to the HVI ability of loading structures up to frequencies that are normally not explored in the standard practice for mechanical dynamic testing. These loads can damage electronic components and sensors mounted on S/C.
An experimental campaign on structural components represents a unique mean of collecting data about the transient behaviour of spacecraft components subjected to HVI threat. The Study is relevant to both "simplified" (i.e. simple plates and sandwich panels made by Aluminium alloy and composite materials) and "complex" (i.e. structural assemblies including joints) targets, hit by projectiles in the range 0.6 - 2.3 mm at velocity from 2 to 5 km/s.
The test-case selected for the experimental activity is the GOCE satellite, whose mission main objective is to measure the Earth's gravity field modelling the geoid with extremely high accuracy and spatial resolution. To do this, it will carry a gradiometer that is sensitive to disturbances, like the one generated by HVI. For this reason, the assessment of the vibration field that propagates after an HVI is fundamental.
As a conclusion, the activity on spacecraft structures resulted in the creation of an extensive database of the disturbance field generated and propagated by HVI on simple and complex assemblies, even highlighting the dependence of the structural response from the mass and velocity of the impacting debris. The disturbance was quantified computing SRS spectra of the measured acceleration signals.
This activity made also possible to evaluate the momentum transferred by the projectiles to the impacted targets. This measurement was necessary to validate the numerical technique used to extrapolate the experimental results to structures and impact conditions different from those achievable at laboratory scale with the existing hypervelocity facilities [28].
Moreover, to investigate in detail the typical features of transient disturbances, a dedicated study was implemented on the application of Wavelet Transform (WT) to the sampled acceleration signal on aluminium simple plates and honeycomb sandwich panels. WT was used to explore the complex wave generation and propagation behaviour inside these targets, thanks to its ability of identifying the following wave features: speed of propagation, type, dispersion properties and frequency content. This work led to a better understanding of the origin of disturbance field due to HVI, demonstrating that WT technique may be used to analyse the elementary constituents of transitory signals.
Referring to the second point, i.e. the study of the collisional evolution of minor bodies of the Solar System, several numerical simulations were carried out to study the wave propagation on planetary-like objects.
HVI characterize the evolutional story of all the small and large bodies of the Solar System. For this reason, the goal of simulations on porous materials (concrete was used as test-case in this thesis) was to obtain a better comprehension of the impact processes and to provide a tool to validate the results of numerical models, through the analysis of wave generation and propagation on different materials. The results of this activity aimed also to contribute to the data interpretation of the ground and space based observations, in particular in view of space missions such as Smart1, MarsExpress, VenusExpress, BepiColombo, Cassini-Huygens, Rosetta, Dawn.
Impact experiments to investigate craterization and catastrophic disruption on planetary objects are limited due to scale effect (i.e. size of the targets, Earth gravity environment, actual performance of the modern hypervelocity facilities). Therefore, a possible method used to study the impact processes is to perform numerical simulations with hydrocodes. The main issue with these tools is the unknown response of materials to high velocity impacts, pressures of several MPa and shock wave propagation. The validation of such models implies to test with the available impact facilities small-scale targets representative of real asteroids and to match experiments and numerical simulations. Waves propagating within the impacted target can be used in the assessment of such numerical models, through the comparison of waves features like: speed, frequency and reflections.
In this thesis the possibility to use an accelerometer to measure waves propagation in concrete spheres (representative of porous targets) and to identify wave features with WT is explored. For this reason, SPH (smooth particles hydrocode) simulations have been carried out on a small-scale concrete sphere to better understand the propagation of shock waves and to evaluate the load effects due to the accelerometer mass. Results show that this measurement is possible, even if it is necessary to perform it with a highly sensitive measurement chain.
10
Alibay, Farah. "Evaluation of multi-vehicle architectures for the exploration of planetary bodies in the Solar System". Thesis, Massachusetts Institute of Technology, 2014. http://hdl.handle.net/1721.1/87476.
Abstract (sommario):
Thesis: Ph. D., Massachusetts Institute of Technology, Department of Aeronautics and Astronautics, 2014.Cataloged from PDF version of thesis.
Includes bibliographical references (pages 193-210).
Planetary exploration missions are becoming increasingly complex and expensive due to ever more ambitious scientific and technical goals. On the other hand, budgets in planetary science have suffered from dramatic cuts over the past decade and projections estimate a flat budget of approximately $1.2B/year for the upcoming years. This has led to a desire for a reduction in the risk and complexity, as well as an increase in the robustness and reliability, of planetary exploration vehicles. One of the methods proposed to deal with this issue is the use of distributed, multi-vehicle architectures as a replacement for the traditional large, monolithic systems used in flagship missions. However, mission concept formulation engineers do not possess the tools to include multi-vehicle architectures in their early trade space exploration process. This is mostly due to the fact that these types of architectures cannot be readily evaluated against monolithic systems through the use of traditional mass-based metrics. Furthermore, in multi-vehicle system, architectural decisions about one vehicle, such as instrument or capability selection, quickly propagate through the entire system and impose requirements on the other vehicles. This can be difficult to model without going through detailed point designs. The objective of this thesis is to explore the potential benefits of both spatially and temporally distributed multi-vehicle systems, where the vehicles are heterogeneous, as compared to monolithic systems. Specifically, a set of metrics mapping the effects of using multi-vehicle systems on science benefit, complexity, mass, cost, coverage, productivity and risk are developed. Furthermore, a software tool to simulate the performance of teams of planetary surface vehicles in their operational environment has been built and its use demonstrated. Finally, the framework put forward in this thesis is used to perform several case studies, including a case study on the exploration of the Jovian moon Europa and another on the ascent and return components of a Mars Sample Return mission. From these, distributed systems are shown to provide increased science return and robustness as well as lower development and manufacturing costs as compared to their monolithic equivalents.
by Farah Alibay.
Ph. D.
11
Schmedemann, Nico [Verfasser]. "On the Chronostratigraphy of Planetary Satellites and Asteroids : Absolute Surface Age Determination of Small Planetary Bodies: Scaling the Lunar Crater Chronology System / Nico Schmedemann". Berlin : Freie Universität Berlin, 2016. http://d-nb.info/108166021X/34.
12
Grimm, Robert E. (Robert Earl). "I. Aspects of lithospheric evolution on Venus. ; II. Thermal and collisional histories of chondrite parent bodies". Thesis, Massachusetts Institute of Technology, 1988. http://hdl.handle.net/1721.1/52901.
13
Person, Michael James. "The use of stellar occultations to study the figures and atmospheres of small bodies in the outer solar system". Thesis, Massachusetts Institute of Technology, 2006. http://hdl.handle.net/1721.1/37278.
Abstract (sommario):
Thesis (Ph. D.)--Massachusetts Institute of Technology, Dept. of Earth, Atmospheric, and Planetary Sciences, 2006.Includes bibliographical references (p. 111-117).
The methods of analyzing stellar occultations by small bodies in the outer solar system are discussed with examples from Triton, Pluto, and Charon. Simulations were performed characterizing the analysis of multi-chord occultations including: the effects of the direction of residual minimization in figure fits, the complications in measuring the reliability of fitted figure parameters when there are few degrees of freedom, and the proper treatment of grazing chords in model fitting. The 2005 July 11 C313.2 stellar occultation by Charon was analyzed. Occultation timings from the three published data sets were combined to accurately determine the mean radius of Charon: 606.0 ± 1.5 km. The analysis indicates that a slight oblateness in the body (0.006 ± 0.003) best matches the data, with a confidence level of 86%. Charon's mean radius corresponds to a bulk density of 1.63 0.07 g/cm3, which is significantly less than Pluto's (1.92 ± 0.12 g/cm3), consistent with an impact formation scenario in which at least one of the impactors was differentiated. The 2002 August 21 P131.1 and the 1988 June 9 P8 stellar occultations by Pluto were analyzed.
(cont.) The ellipticity of Pluto's atmosphere as measured by the P131.1 event is 0.066 ± 0.040, with a Gaussian confidence level of 63%, and the ellipticity as measured by the P8 occultations is 0.091 ± 0.041, with a Gaussian confidence level of 70%. If this non-sphericity is confirmed, its size and variation could possibly be attributed to super-rotating winds driven by sources such as surface frost migration due to changing insolation patterns or albedo properties, gravity waves, and an asymmetric mass distribution in Pluto itself. The 2001 August 23 Tr231 stellar occultation by Triton was analyzed. The half-light radius of Triton's atmosphere was calculated from astrometrically calibrated model fits to the occultation light curve. The resulting half-light radius of 1479.01 km is larger than the value of 1456.3 km derived from the 1997 Trl80 occultation, with a confidence of 77% derived from the uncertainty in the astrometric calibration. If this increase were confirmed, it would indicate that the expansion of Triton's atmosphere detected between the 1989 Voyager 2 observations the 1995 and 1997 stellar occultations by Triton has continued through 2001.
by Michael James Person.
Ph.D.
14
Lomax, Jamie R., John P. Wisniewski, Carol A. Grady, Michael W. McElwain, Jun Hashimoto, Tomoyuki Kudo, Nobuhiko Kusakabe et al. "CONSTRAINING THE MOVEMENT OF THE SPIRAL FEATURES AND THE LOCATIONS OF PLANETARY BODIES WITHIN THE AB AUR SYSTEM". IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/622048.
Abstract (sommario):
We present a new analysis of multi-epoch, H-band, scattered light images of the AB Aur system. We use a Monte Carlo radiative transfer code to simultaneously model the system's spectral energy distribution (SED) and H-band polarized intensity (PI) imagery. We find that a disk-dominated model, as opposed to one that is envelope-dominated, can plausibly reproduce AB Aur's SED and near-IR imagery. This is consistent with previous modeling attempts presented in the literature and supports the idea that at least a subset of AB Aur's spirals originate within the disk. In light of this, we also analyzed the movement of spiral structures in multi-epoch H-band total light and PI imagery of the disk. We detect no significant rotation or change in spatial location of the spiral structures in these data, which span a 5.8-year baseline. If such structures are caused by disk-planet interactions, the lack of observed rotation constrains the location of the orbit of planetary perturbers to be >47 au.
15
Molaro, Jamie. "Stress, on the Rocks: Thermally Induced Stresses in Rocks and Microstructures on Airless Bodies, Implications for Breakdown". Diss., The University of Arizona, 2015. http://hdl.handle.net/10150/593618.
Abstract (sommario):
This dissertation investigates the role of thermomechanical processes in the production of regolith on airless body surfaces. Thermally induced breakdown may provide a significant contribution to their surface evolution, by breaking down rocks and degrading craters. In Chapter 1, we use the traditional terrestrial methodology of evaluating the efficacy of this process by modeling the rate of surface temperature change (dT/dt) on various airless surfaces, using a damage threshold of 2 K/min. We find that the magnitude of dT/dt values is primarily controlled by sunrise/set durations on quickly rotating bodies, such as Vesta, and by distance to the sun on slowly rotating bodies, such as Mercury. The strongest rates of temperature change occur on slopes normal to the sun when a sunrise or sunset occurs, either naturally or because of daytime shadowing. We find, however, that high dT/dt values are not always correlated with high temperature gradients within the surface. This adds to the ambiguity of the poorly understood damage threshold, emphasizes the need further research on this topic that goes beyond the simple 2 K/min criterion. We further investigate this shortcoming in the terrestrial literature in Chapter two by modeling stresses induced by diurnal temperature variations at the mineral grain scale on these bodies. We find that the resulting stresses are controlled by mismatches in material properties between adjacent mineral grains. Peak stresses (on the order of 100s of MPa) are controlled by the coefficient of thermal expansion and Young's modulus of the mineral constituents, and the average stress within the microstructure is determined by relative volume of each mineral. Amplification of stresses occurs at surface-parallel boundaries between adjacent mineral grains and at the tips of pore spaces. We also find that microscopic spatial and temporal surface temperature gradients do not correlate with high stresses, making them inappropriate proxies for investigating microcrack propagation. Although these results provide strong evidence for the significance of thermomechanical processes, more work is needed to quantify crack propagation and rock breakdown rates in order to understand their overall contribution to surface evolution on these bodies. In Chapter 4, we investigate macroscopic scale effects on thermally induced stress fields in boulders of varying sizes and find that macroscopic thermal gradients may play a role in crack propagation within boulder interiors.
16
Vernisse, Yoann Edwin Verfasser], e Karl-Heinz [Akademischer Betreuer] [Glassmeier. "Classification of the interactions of planetary bodies with stellar winds by hybrid simulation / Yoann Edwin Vernisse ; Betreuer: Karl-Heinz Glassmeier". Braunschweig : Technische Universität Braunschweig, 2014. http://d-nb.info/1175820679/34.
17
Burmeister, Steffi [Verfasser], Jürgen [Akademischer Betreuer] Oberst, Jürgen [Gutachter] Oberst e Jürgen [Gutachter] Kusche. "Determining rotational elements of planetary bodies : method and implementation of an inertial frame bundle block adjustment / Steffi Burmeister ; Gutachter: Jürgen Oberst, Jürgen Kusche ; Betreuer: Jürgen Oberst". Berlin : Technische Universität Berlin, 2017. http://d-nb.info/1156271487/34.
18
Ennis, Courtney. "Spectroscopic identification of complex species containing water and ammonia and their importance to icy outer solar system bodies". University of Western Australia. Chemistry Discipline Group, 2009. http://theses.library.uwa.edu.au/adt-WU2009.0110.
Abstract (sommario):
[Truncated abstract] This thesis examines the bonding interactions and chemical processes associated with irradiated water (H2O) and ammonia (NH3) molecules. The experiments conducted in the present study are designed to replicate the surface chemistry of outer Solar System bodies, particularly the icy surfaces of Saturn's inner moons. Infrared (IR) spectroscopy is used to identify the H2ONH3 complex isolated in an argon (Ar) matrix. An electric discharge is then applied to the H2O and NH3 species to produce the hydroxyl-ammonia (OHNH3) complex and the water-amidogen (H2ONH2) complex. Finally, the ammonia-oxygen (NH3O2) complex is formed in an Ar matrix, complementing previous studies performed by the Quickenden research group, which investigated the conversion of OH radicals into molecular O2 on icy planetary surfaces. ... An electric discharge is applied to the NH3 in Ar mixture, producing the NH2 radical subunit of the complex. Two absorption bands are assigned to the H2O subunit vibrational frequencies of the complex; at 1616.1 cm-1 for the ¿2 HOH bending fundamental and at 3532.1 cm-1 for the ¿1 OH bonded stretching fundamental. Two absorption bands are also assigned to the NH2 radical subunit vibrational frequencies of the complex; at 1498.5 cm-1 for the ¿2 HNH bending fundamental and at 3260.8 cm-1 for the ¿3 NH asymmetric stretching fundamental. These assignments are verified by the isotope substitution method, involving the formation of the deuterated D2OND2 complex analogue in an Ar matrix and the measurement of the isotope induced shifts in peak position in the IR region. The isotopic shifts displayed by the IR absorption bands are in good agreement with the theoretically calculated shifts in vibration frequency when going from the H2ONH2 complex fundamentals to the D2OND2 complex fundamentals. The theoretical calculations also derived an interaction energy of 5.2 kcal mol-1 for the HOHNH2 structure of the H2ONH2 complex. This HOHNH2 structure is also confirmed as the preferred structure of the H2ONH2 complex in the IR experiments, by the observation of a large shift in position of the absorption band associated with the H2O subunit ¿1 OH stretching fundamental, away from the position of the H2O monomer ¿1 OH stretching fundamental. This indicates that the H2O subunit donates a hydrogen for the complex bond in the HOHNH2 complex. The NH3O2 complex is identified in solid Ar matrices at 10.5 K by IR analysis. The NH3O2 complex is formed by the co-deposition of gaseous NH3 in Ar mixtures with O2 in Ar gas mixtures. An absorption band is assigned to the ¿1 OO stretching fundamental for the O2 subunit of the NH3O2 complex at 1552.0 cm-1. This assignment is verified by the isotope substitution method, involving the formation of the deuterated ND3O2 complex analogue in an Ar matrix and the measurement of the isotope induced shift in peak position in the IR region. The isotopic shift displayed by the IR absorption band is in good agreement with the theoretically calculated shift in vibration frequency when going from the NH3O2 complex fundamental to the ND3O2 complex fundamental. The theoretical calculations also derived an interaction energy of 0.28 kcal mol-1 for the NH3O2 complex.
19
Nascimento, Sanzia Alves do. "Intera??o estrela planeta: sobre o magnetismo de planetas gigantes gasosos". Universidade Federal do Rio Grande do Norte, 2012. http://repositorio.ufrn.br:8080/jspui/handle/123456789/16620.
Abstract (sommario):
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Previous issue date: 2012-02-16Coordena??o de Aperfei?oamento de Pessoal de N?vel Superior
In this thesis we analyze the effects that the presence of a near gas giant planet can cause in its host star. It has been argued that the star planet interaction can cause changes in the coronal and chromospheric stellar activity. With this in mind, we analyze a sample of 53 extrasolar planets orbiting F, G and K main sequence stars, among them three super-Earths. In this analysis, we look for evidence of changes in the chromospheric activity due to the proximity of the giant planet. We show that, so far, there is not enough evidence to support such a hypothesis. Making use of the same sample and also taking in account available data for the Solar System, we revisit the so-called magnetic Bode s law. This law proposes the existence of a direct relationship between magnetism and rotation. By using estimations for the stellar and planetary magnetic momentM and the angular momentumL, we construct a Blackett s diagram (logL logM). In this diagram is evident that the magnetic Bode s law is valid for both the Solar System and the new planetary systems
Nesta tese s?o analisados os efeitos que a presen?a de um planeta gigante gasoso pr?ximo causa em sua estrela hospedeira. Tem se discutido que a intera??o estrela - planeta possa provocar mudan?as na atividade cromosf?rica e coronal estelar. Tendo isto em mente, analisamos uma amostra composta por 53 planetas extrassolares orbitando estrelas F, G e K da sequ?ncia principal, dentre os quais tr?s superterras. Nesta an?lise, buscamos ind?cios de mudan?as na atividade cromosf?rica estelar devido ? proximidade do planeta gigante. Mostramos que n?o existem evid?ncias suficientes que corroborem tal hip?tese. Fazendo uso desta mesma amostra e de dados dispon?veis na literatura para o Sistema Solar, revisitamos a chamada lei magn?tica de Bode. Esta lei prop?e a exist?ncia de uma rela??o direta entre magnetismo e rota??o. Atrav?s de estimativas para o momento magn?tico M e para o momentum angular L destes objetos, constru?mos e analisamos detalhadamente o diagrama de Blackett (logL logM). Neste diagrama ficou evidente que a lei magn?tica de Bode ? v?lida tanto para o Sistema Solar quanto para os novos sistemas planet?rios
20
Deligny, Cécile. "Origine des éléments volatils et chronologie de leur accrétion au sein du Système Solaire interne : Apport de l'analyse in-situ des achondrites". Electronic Thesis or Diss., Université de Lorraine, 2021. http://www.theses.fr/2021LORR0329.
Abstract (sommario):
Les éléments volatils comme l’hydrogène et l’azote contrôlent l'évolution des corps planétaires et de leurs atmosphères, et sont des éléments essentiels au développement de la vie sur Terre. Néanmoins, l'origine des éléments volatils et la chronologie de leur accrétion par les planètes telluriques formées au sein du système solaire interne restent un sujet de débat et de controverse en sciences planétaires. Pour répondre à ces questions, les rapports isotopiques de l'hydrogène (D/H) et de l'azote (15N/14N) sont des outils puissants pour tracer l'origine (solaire, chondritique ou cométaire) des éléments volatils piégés par les planètes telluriques. Pour contraindre l’origine(s) des éléments volatils piégés par les planètes rocheuses, nous avons donc mesuré les teneurs et les compositions isotopiques de l’hydrogène et de l’azote par microsonde ionique (LGSIMS) dans des achondrites (angrites, météorites maritennes et aubrites) qui proviennent d’astéroïdes différenciés ou de planètes qui sont considérés s’être formés dans le système solaire interne. Ces météorites conservent un enregistrement des étapes initiales de la formation de leurs corps parents et peuvent imposer des contraintes quant à l’évolution précoce des éléments volatils planétaires. L'analyse in-situ par SIMS est une technique quasi-non-destructive, qui permet de mesurer la teneur et la composition isotopique des éléments volatils de différentes phases dans des échantillons terrestres, extraterrestres et synthétiques. Le développement récent du protocole d'analyse de l'azote dans les échantillons silicatés par sonde ionique nous permet de caractériser des objets de la taille d’une dizaine de microns, tels que des inclusions vitreuses. Au cours de cette thèse, les éléments volatils ont été mesurés dans des inclusions magmatiques piégées dans des minéraux et dans les verres interstitiels. Bien que l’analyse de l’azote dans des aubrites n’a pas pu aboutir, les analyses réalisées sur des météorites martiennes et des angrites ont permis de mettre en évidence la présence de quantité importante d’eau et d’azote au sein de ces météorites et de leurs corps parent. En particulier, l’étude des angrites et plus précisément de la météorite D’Orbigny nous a permis de mettre en évidence la présence d’eau et d’azote ayant des compositions isotopiques similaires à celles des météorites primitives formées dans le système solaire externe (i.e., chondrites carbonées de type CM). Ces résultats impliquent que ces éléments volatils étaient présents ~4 millions d’années après la formation des CAIs (i.e., premiers solides à se former dans le système solaire) dans le système solaire interne et ont pu être piégés par les planètes telluriques lors de leur formation. De plus, l’analyses des météorites martiennes et plus particulièrement de Chassigny a révélé la présence d’azote ayant une composition isotopique enrichie en 15N comparée aux chondrites à enstatite et aux diamants terr estres qui sont supposés représenter la valeur la plus primitive de l’azote sur TerreVolatile elements such as hydrogen and nitrogen control the evolution of planetary bodies and their atmospheres, and are essential elements for the development of life on Earth. Nevertheless, the origin of volatile elements and the timing of their accretion by terrestrial planets formed in the inner solar system remains a subject of debate and controversy in planetary science. To answer these questions, the isotopic ratios of hydrogen (D/H) and nitrogen (15N/14N) are powerful tools to trace the origin (solar, chondritic or cometary) of volatile elements trapped in planetary bodies. Therefore, to constrain the source(s) of volatile elements trapped in rocky planets, we analyzed hydrogen and nitrogen contents and isotopic compositions by ion microprobe (LGSIMS) in achondrites that originate from asteroids or from planets that are assumed to have formed in the inner solar system. These meteorites preserve a record of the initial stages of the formation of their parent bodies and can constrain the early evolution of planetary volatile elements. In-situ analysis by SIMS is a quasi-non-destructive technique, which permits to measure the abundance and the isotopic composition of volatile elements of different phases in terrestrial, extraterrestrial and synthetic samples. The recent development of the protocol of nitrogen analysis in silicate samples by ion probe allows us to target tens of micron- sized objects (i.e., glassy melt inclusions). Volatile elements were measured in melt inclusions trapped in minerals and in interstitial glasses. Although the analysis of nitrogen in aubrites was unsuccessful, the analysis performed on Martian meteorites and angrites revealed the presence of a large amount of water and nitrogen within these meteorites. In particular, the study of angrites and more precisely the meteorite D'Orbigny allowed us to highlight the presence of water and nitrogen having isotopic composition similar to those of the primitive meteorites formed in the outer solar system (i.e., CM-like carbonaceous chondrites). These results imply that these volatile elements must have been present in the inner solar system within the first ~4 Ma after CAI formation (i.e., the first solids to form in the solar system) and may have been trapped by the terrestrial planets during their formation. Furthermore, the analysis of Martian meteorites and more particularly of Chassigny revealed the presence of nitrogen with an isotopic composition enriched in 15N compared to enstatite chondrites and terrestrial diamonds which are believed to record the most primitive value of nitrogen on Earth
21
Iagnemma, Karl Dubowsky S. "Mobile robots in rough terrain : estimation, motion planning, and control with application to planetary rovers /". Berlin ; New York : Springer, 2004. http://www.loc.gov/catdir/toc/fy0606/2004106986.html.
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"Isotopic Investigations of Meteoritic Materials: From Earliest-Formed Solids to Planetary Bodies". Doctoral diss., 2016. http://hdl.handle.net/2286/R.I.41284.
Abstract (sommario):
abstract: The beginning of our Solar System, including events such as the formation of the first solids as well as the accretion and differentiation of planetary bodies, is recorded in meteoritic material. This record can be deciphered using petrographic, geochemical and isotopic investigations of different classes of meteorites and their components. In this dissertation, I have investigated a variety of isotope systematics in chondritic and achondritic meteorites to understand processes that have shaped our Solar System. Specifically, the investigations conducted here are in two main areas: 1) Hydrogen isotope systematics in a meteorite representing the freshest known sample of the martian crust, and 2) Isotopic studies (specifically relating to high resolution chronology, nucleosynthetic anomalies and mass-dependent fractionations) in calcium-aluminum-rich inclusions, which are thought to be the earliest-formed solids in the Solar System. Chapter 1 of this dissertation presents a review of the hydrogen isotopic compositions of various planetary bodies and reservoirs in the Solar System, which could serve as tracers for the volatile sources. Chapter 2 focuses on an investigation of the hydrogen isotopic systematics in the freshest martian meteorite fall, Tissint, using the Cameca IMS-6f secondary ion mass spectrometer (SIMS). These first two chapters comprise the first part of this dissertation. The second part is comprised of chapters 3 through 6 and is focused on isotopic analyses of Calcium-Aluminum-rich Inclusions (CAIs). Chapter 3 is a review of CAIs, which record some of the earliest processes that occurred in the solar nebula. Chapter 4 presents the results of an investigation of the 26Al-26Mg short-lived chronometer (half-life ~0.72 Ma) in two CAIs and their Wark-Lovering (WL) rims from a CV3 carbonaceous chondrite using the Cameca NanoSIMS 50L. Chapter 5 is focused on the results of a study of the Zr isotope compositions of a suite of 15 CAIs from different carbonaceous chondrites using multicollector inductively coupled plasma mass spectrometry (MC-ICPMS), in order to identify nucleosynthetic anomalies in the CAI-forming region. Chapter 6 focuses on the mass-dependent Mg isotopic compositions measured in 11 CAIs from the Allende CV3 carbonaceous chondrite using MC-ICPMS, to evaluate effects of thermal processing on CAIs.Dissertation/Thesis
Doctoral Dissertation Geological Sciences 2016
23
Masoumzadeh, Jouzdani Nafiseh. "Surface reflectance analysis of small bodies on different scales". Doctoral thesis, 2015. http://hdl.handle.net/11858/00-1735-0000-0022-6075-E.
24
Liao, Chen-yuan, e 廖振淵. "A Study of Magnetic Polishing for SUS304 Curve Surface with Planetary Bodies Combined Two-Dimensional Vibration". Thesis, 2013. http://ndltd.ncl.edu.tw/handle/73817624674849029840.
Abstract (sommario):
碩士國立中央大學
機械工程學系在職專班
101
Abstract The normal vibration directions of vibration-assisted magnetic abrasive finishing are all parallel or perpendicular to the surface of workpiece. It’s shortcomings are easily lead to more scratches on the surface, and difficult to obtain mirror effect. A study of magnetic polishing for SUS304 with planetary bodies combined two-dimensional vibration. The main purpose of the planetary bodies of rotation and revolution characteristics, excellent surface morphology, and saving energy and time can also be reached. Series of experiments by controlling the working gap, the amplitude of the vibration platform, steel particle size and so on. This mechanism can enhance the surface quality and efficiency. Taguchi experiment show that the combination of better parameters for the surface improvement : working gap 1 mm, the amplitude of the vibration platform 0.1mm, steel particle size of 0.125 mm , SiC weight of 3 g, steel weight of 0.5 g * 2, the weight of the slurry 5g, vibration platform frequency of 16.667Hz, magnet pole rotational speed 500 rpm (156). For the curve improvement : working gap 0.5 mm, the amplitude of the vibration platform 0.1mm, steel particle size of 0.125 mm , SiC weight of 3 g, steel weight of 0.5 g * 2, the weight of the slurry 5g, vibration platform frequency of 16.667Hz, magnet pole rotational speed 500 rpm (156). This mechanism can be effective in improving the stainless surface S.R. from Ra 0.23 μm to 0.058 μm, improvement rate was 74% and improving the stainless curve S.R. from Ra 0.23 μm to 0.058 μm, improvement rate was 74%. which can prove that planetary bodies combination of the two-dimensional vibration support mechanisms to improve quality. Keywords: planetary bodies, two-dimensional vibration, polished stainless steel, rotation and revolution.
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"Planetary Geological Science and Aerospace Systems Engineering Applications of Thermal Infrared Remote Sensing for Earth, Mars, and the Outer Bodies". Doctoral diss., 2018. http://hdl.handle.net/2286/R.I.50586.
Abstract (sommario):
abstract: Many planetary science missions study thermophysical properties of surfaces using infrared spectrometers and infrared cameras. Thermal inertia is a frequently derived thermophysical property that quantifies the ability for heat to exchange through planetary surfaces.
To conceptualize thermal inertia, the diffusion equation analogies are extended using a general effusivity term: the square root of a product of conductivity and capacity terms. A hypothetical thermal inductance was investigated for diurnal planetary heating. The hyperbolic heat diffusion equation was solved to derive an augmented thermal inertia. The hypothetical thermal inductance was modeled with negligible effect on Mars.
Extending spectral performance of infrared cameras was desired for colder bodies in the outer solar system where peak infrared emission is at longer wavelengths. The far-infrared response of an infrared microbolometer array with a retrofitted diamond window was determined using an OSIRIS-REx—OTES interferometer. An instrument response function of the diamond interferometer-microbolometer system shows extended peak performance from 15 µm out to 20 µm and 40% performance to at least 30 µm. The results are folded into E-THEMIS for the NASA flagship mission: Europa Clipper.
Infrared camera systems are desired for the expanding smallsat community that can inherit risk and relax performance requirements. The Thermal-camera for Exploration, Science, and Imaging Spacecraft (THESIS) was developed for the Prox-1 microsat mission. THESIS, incorporating 2001 Mars Odyssey—THEMIS experience, consists of an infrared camera, a visible camera, and an instrument computer. THESIS was planned to provide images for demonstrating autonomous proximity operations between two spacecraft, verifying deployment of the Planetary Society’s LightSail-B, and conducting remote sensing of Earth. Prox-1—THESIS was selected as the finalist for the competed University Nanosatellite Program-7 and was awarded a launch on the maiden commercial SpaceX Falcon Heavy. THESIS captures 8-12 µm IR images with 100 mm optics and RGB color images with 25 mm optics. The instrument computer was capable of instrument commanding, automatic data processing, image storage, and telemetry recording. The completed THESIS has a mass of 2.04 kg, a combined volume of 3U, and uses 7W of power. THESIS was designed, fabricated, integrated, and tested in ASU’s 100K clean lab.Dissertation/Thesis
Doctoral Dissertation Geological Sciences 2018
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POGGIALI, VALERIO. "Observations of Titan liquid bodies by means of the Cassini RADAR altimeter". Doctoral thesis, 2017. http://hdl.handle.net/11573/938037.
Abstract (sommario):
Twenty years after its great departure from Cape Canaveral the Cassini mission is going to have the “Grand Finale” it deserves. This spacecraft definitely marked a milestone in astronautical history as one of the best examples of collaboration among different space agencies (NASA-ESA-ASI) and a great model for any other future mission for planetary exploration. A discovery machine that unveiled the Titan’s lively world and that doesn’t stop giving surprises at every new observation. I’m Valerio Poggiali, phD candidate, and with my colleagues and professors of La Sapienza University of Rome I’m involved in the Cassini RADAR altimeter data processing, a task bequeathed to us by our Prof. Emeritus Giovanni Picardi who started believing in this project already at the beginning of nineties when he published a paper entitled “The Radar System for the Exploration of Titan”. It is 1992, and he states: “the knowledge of the ocean depth is particularly important and its determination is one of the main requirements for the radar instrument”. Actually he announced twenty-two years in advance our work on “The Bathymetry of a Titan Sea” in which we reported about an incredible observation made by the Cassini radar altimeter on May 23st, 2013. We were waiting for that fly-by by years as it was representing the only opportunity to test the instrument capability to plumb the bottom of a Titan sea and infer about its dielectric properties (besides proving once for all the liquid nature of those dark features). After Kraken and before Punga, the Ligeia Mare is the second greatest sea of Titan (roughly 260 x 217 miles). We have been able to track a deepest point of 180 yards and estimate its liquid to be composed by an extremely pure mixture of liquid hydrocarbons (laboratory experiments at JPL eventually confirmed components to be methane, ethane and nitrogen). The following period has been very busy for us, but also extremely rewarding. After the publication of Ligeia Mare bathymetry, the Cassini radar altimeter observed the Kraken Mare on August 21st, 2014 and the Punga Mare on January 11st, 2015. The measurements we had to perform were very challenging. Main difficulties came from the necessity to track the subsurface also in the shallowest parts of seas where we have to push the radar capabilities to the limits of its vertical resolution (nominally 33 yards but with some super-resolution algorithms improvable of a factor of about two). Another great test that we faced was in the production of the bathymetry of the largest lake (43 x 124 miles) of the southern polar area of Titan, the Ontario Lacus. The severe saturation of the receiver united to the shallowness of this liquid body (preliminary results suggested a 50 yards maximum depth along the altimeter ground track, that of course could be not the deepest point) imposed the necessity of developing a different method for determine its bathymetry and dielectric properties. Also if the Cassini radar will not observe Titan seas anymore (we will have just a last look to northern polar small lakes during Cassini’s last flyby of Titan on April 2017) we have still many analyses to perform on the already collected data, these will engage us for years to come. The more Cassini mission will come closer to its end on September 15, 2017, the more we will have to stay tuned to not miss anyone of the discoveries that will certainly follow as the spacecraft will finally approach Saturn, receiving, as if it was an engagement gift, the unique opportunity of a closer observation of its precious rings.
In this PhD dissertation I would like to resume the main steps we followed for analyzing the Cassini radar altimeter data from which we obtained the first bathymetries of extraterrestrial liquid bodies, starting from a brief introduction to the RADAR instrument characteristics and its capabilities. Later I will focus on the backscattering models we adopted in order to effectively interpret the radar altimeter nadiral power returns from the surface of Titan.
A detailed description will follow of the simulator we developed in order to reconstruct as accurately as possible how the Cassini radar receiving chain processes on board the incoming signal. Then, I will describe the results we obtained on Ligeia Mare and Ontario Lacus, giving some anticipations on the work ongoing for Punga and Kraken Mare.
The last part will be finally dedicated to our discovery on Titan of liquid-filled canyons directly connected to seas. I will describe how the radar altimeter was able to measure their depth and infer about their nature of sea flooded valleys by means of a comparison of the levels of their liquids.
Far from being just a library-based theoretical dissertation, this document will intentionally focus on the work we carried out and on the consequent results we obtained in the framework of the Cassini mission. The techniques described herein and, in particular, the simulator and the Bayesian method for the estimation of unknown parameters we adopted for this work are the result of the fruitful collaboration between our Dipartimento di Ingegneria Elettronica e Telecomunicazioni (DIET) of “La Sapienza” University of Rome and the Astronomy department of the Cornell University in Ithaca (NY).
27
Lantukh, Demyan Vasilyevich. "Preliminary design of spacecraft trajectories for missions to outer planets and small bodies". Thesis, 2015. http://hdl.handle.net/2152/31341.
Abstract (sommario):
Multiple gravity assist (MGA) spacecraft trajectories can be difficult to find, an intractable problem to solve completely. However, these trajectories have enormous benefits for missions to challenging destinations such as outer planets and primitive bodies. Techniques are presented to aid in solving this problem with a global search tool and additional investigation into one particular proximity operations option is discussed. Explore is a global grid-search MGA trajectory pathsolving tool. An efficient sequential tree search eliminates v∞ discontinuities and prunes trajectories. Performance indices may be applied to further prune the search, with multiple objectives handled by allowing these indices to change between trajectory segments and by pruning with a Pareto-optimality ranking. The MGA search is extended to include deep space maneuvers (DSM), v∞ leveraging transfers (VILT) and low-thrust (LT) transfers. In addition, rendezvous or nπ sequences can patch the transfers together, enabling automatic augmentation of the MGA sequence. Details of VILT segments and nπ sequences are presented: A boundaryvalue problem (BVP) VILT formulation using a one-dimensional root-solve enables inclusion of an efficient class of maneuvers with runtime comparable to solving ballistic transfers. Importantly, the BVP VILT also allows the calculation of velocity-aligned apsidal maneuvers (VAM), including inter-body transfers and orbit insertion maneuvers. A method for automated inclusion of nπ transfers such as resonant returns and back-flip trajectories is introduced: a BVP is posed on the v∞ sphere and solved with one or more nπ transfers – which may additionally fulfill specified science objectives. The nπ sequence BVP is implemented within the broader search, combining nπ and other transfers in the same trajectory. To aid proximity operations around small bodies, analytical methods are used to investigate stability regions in the presence of significant solar radiation pressure (SRP) and body oblateness perturbations. The interactions of these perturbations allow for heliotropic orbits, a stable family of low-altitude orbits investigated in detail. A novel constrained double-averaging technique analytically determines inclined heliotropic orbits. This type of knowledge is uniquely valuable for small body missions where SRP and irregular body shape are very important and where target selection is often a part of the mission design.
28
Millar, Candida Sharon. "Wellness pastoral care and women with new babies". Thesis, 2003. http://hdl.handle.net/10500/1238.
Abstract (sommario):
As participants, we agreed that women's silenced voices need to be heard, more specific to this participatory action research, the voices of women with new babies.
Through wellness pastoral care, we co-laboured in finding ways of standing up to prescribed religious and cultural ideas regarding womaness and motherhood. Pastoral care in partnership with feminist theology and mutuality in community opened a safe place to renegotiate our own preferred ways of seeing our bodies, selves, sexuality, and womaness.
The pastoral care, counselling, and mutuality experienced as a research group became the prevalent characteristic of our wellness that we wished to extend beyond the group and into families, churches, community cohorts, and the planet.
This research is one platform on which the participating women shared hurts, found a place to be heard, and having come to know our Self more deeply, offer this Self as a gift to the reader.Practical Theology
M.Th.
29
Pohl, Leoš. "Rovnice vedení tepla a termofyzikální modelování planetek". Master's thesis, 2014. http://www.nusl.cz/ntk/nusl-336583.
Abstract (sommario):
Light curve inversion is a standard method to determine shapes, rotation periods and spin axis orientations of asteroids. This method can be extended to determine the size, albedo, thermal inertia and surface roughness parameters of an asteroid by including observations in thermal infrared. A solution of the Heat Conduction Equation (HCE) is necessary to model infrared flux from the asteroid. We analyse the accuracy requirements of the extended method for numerical solution of the HCE. We show that current implementation leads to errors in flux that are substantial. We recommend changes in the current implementation of the HCE solving approach to address the accuracy issues. We discuss uniqueness and stability of the solutions produced by the extended method as well as the accuracy of the determined parameters and their stability. Shapes of asteroids are produced and their physical attributes are determined based on light curve and infrared data.