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The topics addressed are: (1) summary of design requirements; (2) spacecraft system design; (3) subsystem design; (4) spacecraft performance; (5) mission performance of the Jupiter orbiter; and (6) mission performance of the Saturn orbiter. The results presented in this report show that the baseline Pioneer F/G spacecraft design can be readily adapted, with some modifications, to the requirements of Jupiter and Saturn orbit missions. The spacecraft would be launched by the Titan 3 E/Centaur/TE 364-4, which presents a launch environment and interfaces comparable to the Atlas/Centaur/TE 364-4 that was used for the Pioneer 10 and 11 Jupiter flyby missions, except for providing a larger (14-foot) standard payload fairing.

We compare International Ultraviolet Explorer (IUE) spectral observations of Jupiter's UltraViolet (UV) aurora in H-Lyman alpha (H-Lya) and H2 emissions with images of the UV aurora with HST to make more realistic interpretations of the IUE dataset. Use the limited spatial information in the IUE line-by-line spectra of the bright H-Lya line emission in the form of pseudo-monochromatic images at the IUE 3.5 arcsec resolution (Lya pseudo-images), to derive information on the emissions. Analysing of H2 spectra of Saturn's UV aurora to infer atmospheric level of auroral excitation from the methane absorption (color ratios). Analysing of a Uranus IUE dataset to determine periodicity in the emissions attributable to auroral emission fixed in magnetic longitude. Reviewing of the results from IUE observations of the major planets, upper atmospheres and interactions with the planets magnetospheres. Analysing of IUE spectra of the UV emissions from Io to identify excitation processes and infer properties of the Io-torus-Jupiter system.

Using novel spectropolarimeteric imaging techniques, researchers have studied the outer planets, Titan, and various comets. In the previous year, researchers submitted and have now in press or published fourteen papers on studies of comets and planets, as well as instrumentation developments to enhance observational studies.

The work performed by the magnetic fields investigation team during the mission definition phases of the Outer Planets Grand Tour (OPGT) and the Mariner Jupiter Saturn (MJS) Missions is reported. This work involved three tasks: (1) defining the objectives of the magnetic fields investigations, (2) defining the magnetometer systems required to meet these objectives, and (3) developing and testing hardware elements in certain mission-specific areas.

The work is reported of the Photopolarimetry Team in identifying scientific objectives for photometer/polarimeter experiments for outer planet flyby missions. A discussion of the scientific objectives which can be attained with a photometer/polarimeter experiment, and summaries of the special studies which were performed for the Photopolarimetry Team are presented along with a description of the photometer/polarimeter design which was developed for the Meteoroid Detection Team.

A mod designed to add rings and moons to Neidon. (REQUIRES OPM) Homepage: https://forum.kerbalspaceprogram.com/topic/225300-112x-planet-pack-outer-planets-expansion-opx/ Repository: https://github.com/TheWhistleGang/OPX-NeidonPlus License(s): MIT

Technical facts about this news release: About the Object Object Name: Uranus; Neptune Object Description: Planets Distance: The semi-major axis of Uranus's orbit about the sun is 19.18 Astronomical Units (A.U.) or roughly 2.9 billion km. The semi-major axis of Neptune's orbit about the Sun is 30.06 Astronomical Units (A.U.) or roughly 4.5 billion km. Dimensions: Uranus (without rings) has a diameter of roughly 32,000 miles (51,000 km) at the equator.Neptune has a diameter of roughly 30,800 miles (49,600 km) at the equator. About the Data Object: Uranus Uranus Neptune Instrument: ACS/HRC STIS/CCD STIS/CCD HST Programs: 9725: E. Karkoschka and M. Tomasko (U. AZ) 9035: E. Karkoschka (U. AZ), M. Lemmon (Texas A&M), M. Tomasko (U. AZ) 9330: E. Karkoschka (U. AZ), M. Lemmon (Texas A&M), M. Tomasko (U. AZ) Exposure Date(s): August 30, 2003 August 19, 2002 August 3, 2003 Filters: F435W, F550M, F658N, F660N, F775W, F814W, F850LP, and F892N G430L and G750L G430L, G750L, CLEAR, and F28X50LP "Note:" Uranus images within this press release were taken with ACS/HRC. They were color calibrated using STIS/CCD data of Uranus. Neptune images within this press release were taken with STIS/CCD. About the Image Image Credit: NASA and E. Karkoschka (University of Arizona) Release Date: January 22, 2004 Orientation: Rings and Moons Circling Uranus [ http://imgsrc.hubblesite.org/hu/db/2004/05/images/a/formats/compass_large_web.jpg ] Neptune as Seen with Color Filters [ http://imgsrc.hubblesite.org/hu/db/2004/05/images/b/formats/compass_large_web.jpg ] *News Release Number:*: STScI-2004-05d

Expands the Kerbol system with new planets and moons based on Saturn, Uranus, Neptune and their moons Homepage: http://forum.kerbalspaceprogram.com/threads/104280-0-90-Outer-Planet-Mods-Expands-the-Kerbol-system-with-new-planets-based-on-Saturn License(s): CC-BY-NC-SA-4.0

The Outer Planets Mod is a mod that expands the outer edges of the Kerbol system to create something akin to the real Solar System's. Homepage: https://forum.kerbalspaceprogram.com/index.php?/topic/165854-k Repository: https://github.com/Poodmund/Outer-Planets-Mod License(s): CC-BY-NC-SA-4.0

Technical facts about this news release: About the Object Object Name: Uranus; Neptune Object Description: Planets Distance: The semi-major axis of Uranus's orbit about the sun is 19.18 Astronomical Units (A.U.) or roughly 2.9 billion km. The semi-major axis of Neptune's orbit about the Sun is 30.06 Astronomical Units (A.U.) or roughly 4.5 billion km. Dimensions: Uranus (without rings) has a diameter of roughly 32,000 miles (51,000 km) at the equator.Neptune has a diameter of roughly 30,800 miles (49,600 km) at the equator. About the Data Object: Uranus Uranus Neptune Instrument: ACS/HRC STIS/CCD STIS/CCD HST Programs: 9725: E. Karkoschka and M. Tomasko (U. AZ) 9035: E. Karkoschka (U. AZ), M. Lemmon (Texas A&M), M. Tomasko (U. AZ) 9330: E. Karkoschka (U. AZ), M. Lemmon (Texas A&M), M. Tomasko (U. AZ) Exposure Date(s): August 30, 2003 August 19, 2002 August 3, 2003 Filters: F435W, F550M, F658N, F660N, F775W, F814W, F850LP, and F892N G430L and G750L G430L, G750L, CLEAR, and F28X50LP "Note:" Uranus images within this press release were taken with ACS/HRC. They were color calibrated using STIS/CCD data of Uranus. Neptune images within this press release were taken with STIS/CCD. About the Image Image Credit: NASA and E. Karkoschka (University of Arizona) Release Date: January 22, 2004 Orientation: Rings and Moons Circling Uranus [ http://imgsrc.hubblesite.org/hu/db/2004/05/images/a/formats/compass_large_web.jpg ] Neptune as Seen with Color Filters [ http://imgsrc.hubblesite.org/hu/db/2004/05/images/b/formats/compass_large_web.jpg ] *News Release Number:*: STScI-2004-05b

Technical facts about this news release: About the Object Object Name: Uranus; Neptune Object Description: Planets Distance: The semi-major axis of Uranus's orbit about the sun is 19.18 Astronomical Units (A.U.) or roughly 2.9 billion km. The semi-major axis of Neptune's orbit about the Sun is 30.06 Astronomical Units (A.U.) or roughly 4.5 billion km. Dimensions: Uranus (without rings) has a diameter of roughly 32,000 miles (51,000 km) at the equator.Neptune has a diameter of roughly 30,800 miles (49,600 km) at the equator. About the Data Object: Uranus Uranus Neptune Instrument: ACS/HRC STIS/CCD STIS/CCD HST Programs: 9725: E. Karkoschka and M. Tomasko (U. AZ) 9035: E. Karkoschka (U. AZ), M. Lemmon (Texas A&M), M. Tomasko (U. AZ) 9330: E. Karkoschka (U. AZ), M. Lemmon (Texas A&M), M. Tomasko (U. AZ) Exposure Date(s): August 30, 2003 August 19, 2002 August 3, 2003 Filters: F435W, F550M, F658N, F660N, F775W, F814W, F850LP, and F892N G430L and G750L G430L, G750L, CLEAR, and F28X50LP "Note:" Uranus images within this press release were taken with ACS/HRC. They were color calibrated using STIS/CCD data of Uranus. Neptune images within this press release were taken with STIS/CCD. About the Image Image Credit: NASA and E. Karkoschka (University of Arizona) Release Date: January 22, 2004 Orientation: Rings and Moons Circling Uranus [ http://imgsrc.hubblesite.org/hu/db/2004/05/images/a/formats/compass_large_web.jpg ] Neptune as Seen with Color Filters [ http://imgsrc.hubblesite.org/hu/db/2004/05/images/b/formats/compass_large_web.jpg ] *News Release Number:*: STScI-2004-05e

Originally uploaded by VintageCG on August 26, 2009. https://www.youtube.com/watch?v=M92Kx4iXG0M A JPL retrospective of the Voyager I and II "Grand Tour" of the outer planets, including many of James Blinn's famous CG flyby simulations. Very inspirational! THIS IS SCIENCE!

We tabulate the most abundant gases and their radiation yields, for two experimental pressures: 0.24 mb, more relevant to upper atmosphere excitation, and 17 mb, more relevant to tropospheric, cosmic ray excitation. The yields computed in the 0.24 mb experiment combined with measured electronic fluxes and a simple, eddy diffusion model of Titan's atmosphere predict abundances of detected molecules in agreement with those found by Voyager and for heavier products, in somewhat better agreement with observation than photochemical absolute reaction rate kinetics models. All Voyager organics are accounted for and no detectable products are found that Voyager did not detect. A striking increase of products with multiple bonds is found with decreasing pressure. Hydrocarbon abundances decline slowly with increasing carbon number. Additionally, we list preliminary estimates for the yield of the heteropolymer, which seems to be produced in a quantity comparable (in moles of CN consumed) to the total amount of gaseous product. The production rate required to sustain Titan's haze against sedimentation also indicates yields of this order. As can be seen from the table, over 10(exp 9) years substantial amounts of these products can accumulate on the surface -- ranging from cm thickness for the (CN equals 4) species to a meter or more for HCN and C2H2; we also expect a meter or more of tholins. Similar analyses have been or are being done for the Jovian planets and Triton. Charged particle irradiation of hydrocarbon clathrates or mixed hydrocarbon/water ices produces a range of organic products, reddening and darkening of the ices and characteristic infrared spectra. From such spectra, the predicted emission by fine particles in cometary comae well-matches the observed 3.4 micron emission spectra of Comet Halley and other recent comets. Heliocentric evolution of organic emission features in comets is predicted. Organic products of such ice irradiation may account for colors and albedos on some of the satellites in the outer solar system, especially Triton and Pluto, where solid methane is known to exist.

Expands the Kerbol system with new planets and moons based on Saturn, Uranus, Neptune and their moons Homepage: http://forum.kerbalspaceprogram.com/threads/104280-0-90-Outer-Planet-Mods-Expands-the-Kerbol-system-with-new-planets-based-on-Saturn License(s): CC-BY-NC-SA-4.0

The Outer Planets Mod is a mod that expands the outer edges of the Kerbol system to create something akin to the real Solar System's. Homepage: https://forum.kerbalspaceprogram.com/index.php?/topic/184789-* Repository: https://github.com/Poodmund/Outer-Planets-Mod License(s): CC-BY-NC-SA-4.0

A quadrifilar helix antenna was selected for the Pioneer spacecraft receiving antenna. A model was constructed for radiation pattern measurement at 2.2 GHz. Radiation patterns were measured with the model quadrifilar helix antenna mounted on a Pioneer spacecraft model and four different configurations were tested. The results show that the antenna location does not have a major effect on its patterns over the aft hemisphere but moving the antenna away from the spacecraft improves the antenna performance.

The principal objective is presented of the UV observations, with emphasis placed on hydrogen and helium. Calculations are given for airglow and occultation. Mission requirements and trajectories are also reported for future observations.

The atmospheric absorption that exists in the atmospheres of the major outer planets, Jupiter, Saturn, and Uranus is discussed along with system noise temperature problems at Jupiter.

A space based coronagraph, whether as part of the WFIRST/AFTA mission or on a dedicated space telescope such as Exo-C or -S, will be able to obtain photometry and spectra of multiple gas giant planets around nearby stars, including many known from radial velocity detections. Such observations will constrain the masses, atmospheric compositions, clouds, and photochemistry of these worlds. Giant planet albedo models, such as those of Cahoy et al. (2010) and Lewis et al. (this meeting), will be crucial for mission planning and interpreting the data. However it is equally important that insights gleaned from decades of solar system imaging and spectroscopy of giant planets be leveraged to optimize both instrument design and data interpretation. To illustrate these points we will draw on examples from solar system observations, by both HST and ground based telescopes, as well as by Voyager, Galileo, and Cassini, to demonstrate the importance clouds, photochemical hazes, and various molecular absorbers play in sculpting the light scattered by solar system giant planets. We will demonstrate how measurements of the relative depths of multiple methane absorption bands of varying strengths have been key to disentangling the competing effects of gas column abundances, variations in cloud height and opacity, and scattering by high altitude photochemical hazes. We will highlight both the successes, such as the accurate remote determination of the atmospheric methane abundance of Jupiter, and a few failures from these types of observations. These lessons provide insights into technical issues facing spacecraft designers, from the selection of the most valuable camera filters to carry to the required capabilities of the flight spectrometer, as well as mission design questions such as choosing the most favorable phase angles for atmospheric characterization.

The Outer Planets Mod is a mod that expands the outer edges of the Kerbol system to create something akin to the real Solar System's. Homepage: https://forum.kerbalspaceprogram.com/index.php?/topic/165854-k Repository: https://github.com/Poodmund/Outer-Planets-Mod License(s): CC-BY-NC-SA-4.0

No abstract available

Feasibility study of symmetric round trip flybys to outer planets

Outer Planets Mod is a mod that expands the outer edges of the Kerbol system, to create something akin to the real Solar System's. It adds Kerbalized versions of Saturn, Uranus, Neptune and Pluto, just like real-life. these faraway planets and moons provide a challenge rarely encountered in Kerbal Space Program. You'll have to figure out new transfer windows, provide your spacecraft with more Delta-V and be ready to travel years or even decades. Homepage: http://forum.kerbalspaceprogram.com/index.php?/topic/93999-105-outer-planets-mod-192-customasteroids-support-loadondemand-and-many-bug-fixes-17-jan/ License(s): CC-BY-NC-SA-4.0

Outer Planets Mod is a mod that expands the outer edges of the Kerbol system, to create something akin to the real Solar System's. It adds Kerbalized versions of Saturn, Uranus, Neptune and Pluto, just like real-life. these faraway planets and moons provide a challenge rarely encountered in Kerbal Space Program. You'll have to figure out new transfer windows, provide your spacecraft with more Delta-V and be ready to travel years or even decades. Homepage: http://forum.kerbalspaceprogram.com/index.php?/topic/93999-105-outer-planets-mod-192-customasteroids-support-loadondemand-and-many-bug-fixes-17-jan/ License(s): CC-BY-NC-SA-4.0

The Outer Planets Mod is a mod that expands the outer edges of the Kerbol system to create something akin to the real Solar System's. Homepage: https://forum.kerbalspaceprogram.com/index.php?/topic/165854-k Repository: https://github.com/Poodmund/Outer-Planets-Mod License(s): CC-BY-NC-SA-4.0

The Outer Planets Mod is a mod that expands the outer edges of the Kerbol system to create something akin to the real Solar System's. Homepage: https://forum.kerbalspaceprogram.com/index.php?/topic/184789-* Repository: https://github.com/Poodmund/Outer-Planets-Mod License(s): CC-BY-NC-SA-4.0

The Outer Planets Mod is a mod that expands the outer edges of the Kerbol system to create something akin to the real Solar System's. Homepage: https://forum.kerbalspaceprogram.com/index.php?/topic/184789-* Repository: https://github.com/Poodmund/Outer-Planets-Mod License(s): CC-BY-NC-SA-4.0

63 pages

We present results from a high-contrast adaptive optics imaging search for giant planets and brown dwarfs (>1 MJup) around 122 newly identified nearby (

We present results from a high-contrast adaptive optics imaging search for giant planets and brown dwarfs (>1 MJup) around 122 newly identified nearby (

NASA (National Aeronautics and Space Administration): Voyagers to the Outer Planets: Volume 8 - Jupiter. Selected Images in Range 20626.29 - 20863.06 in Compressed Format. Selected Images in Range 13854.55 - 20863.06 in Browse Format. Part of Planetary Data Systems. From Reference Technology, Inc. USA_NASA_PDS_VG_0008. October 1989.

48p. :

Four related tasks are discussed for data transmission from a probe prior to entering the atmosphere of Jupiter to an orbiting spacecraft in a trajectory past the planet: (1) link analysis and design; (2) system conceptual design; (3) Doppler measurement analysis; and (4) an electronically despun antenna. For tasks 1, 3, and 4, an analytical approach was developed and combined with computational capability available to produce quantitative results corresponding to requirements and constraints given by NASA, ARC. One constraint having a major impact on the numerical results of the link analysis was the assumption of a nonsteerable antenna on a spinning orbiter. Other constraints included the interplanetary trajectory and the approach trajectory. Because the Jupiter Orbiter Probe (JOP) program is currently in a state of evolution, all requirements and constraints applied during this study are subject to change. However, the relationships of parameters as developed will remain valid and will aid in planning Jupiter missions.

Four related tasks are discussed for data transmission from a probe prior to entering the atmosphere of Jupiter to an orbiting spacecraft in a trajectory past the planet: (1) link analysis and design; (2) system conceptual design; (3) Doppler measurement analysis; and (4) an electronically despun antenna. For tasks 1, 3, and 4, an analytical approach was developed and combined with computational capability available to produce quantitative results corresponding to requirements and constraints given by NASA, ARC. One constraint having a major impact on the numerical results of the link analysis was the assumption of a nonsteerable antenna on a spinning orbiter. Other constraints included the interplanetary trajectory and the approach trajectory. Because the Jupiter Orbiter Probe (JOP) program is currently in a state of evolution, all requirements and constraints applied during this study are subject to change. However, the relationships of parameters as developed will remain valid and will aid in planning Jupiter missions.

The Outer Planet Assessment Group (OPAG) recommends the DS support the JEO and EJSM flagship endorse the Cassini Solstice Mission support technology to enable a major mission to Titan/Enceladus examine small flagship missions and assess the feasibilty of a defined set of NF candidates.

The Outer Planet Assessment Group (OPAG) recommends the DS support the JEO and EJSM flagship endorse the Cassini Solstice Mission support technology to enable a major mission to Titan/Enceladus examine small flagship missions and assess the feasibilty of a defined set of NF candidates.

The Outer Planet Assessment Group (OPAG) recommends the DS support the JEO and EJSM flagship endorse the Cassini Solstice Mission support technology to enable a major mission to Titan/Enceladus examine small flagship missions and assess the feasibilty of a defined set of NF candidates.

In this paper we investigate the effects that an anomalous acceleration as that experienced by the Pioneer spacecraft after they passed the 20 AU threshold would induce on the orbital motions of the Solar System planets placed at heliocentric distances of 20 AU or larger as Uranus, Neptune and Pluto. It turns out that such an acceleration, with a magnitude of 8.74\times 10^-10 m s^-2, would affect their orbits with secular and short-period signals large enough to be detected according to the latest published results by E.V. Pitjeva, even by considering errors up to 30 times larger than those released. The absence of such anomalous signatures in the latest data rules out the possibility that in the region 20-40 AU of the Solar System an anomalous force field inducing a constant and radial acceleration with those characteristics affects the motion of the major planets.

In this paper we investigate the effects that an anomalous acceleration as that experienced by the Pioneer spacecraft after they passed the 20 AU threshold would induce on the orbital motions of the Solar System planets placed at heliocentric distances of 20 AU or larger as Uranus, Neptune and Pluto. It turns out that such an acceleration, with a magnitude of 8.74\times 10^-10 m s^-2, would affect their orbits with secular and short-period signals large enough to be detected according to the latest published results by E.V. Pitjeva, even by considering errors up to 30 times larger than those released. The absence of such anomalous signatures in the latest data rules out the possibility that in the region 20-40 AU of the Solar System an anomalous force field inducing a constant and radial acceleration with those characteristics affects the motion of the major planets.

Includes bibliographical references (p. 261-271) and index

Includes bibliographical references (p. 261-271) and index

Includes bibliographical references (p. 261-271) and index

*Description*: Atmospheric features on Uranus and Neptune are revealed in images taken with the Space Telescope Imaging Spectrograph and the Advanced Camera for Surveys aboard NASA's Hubble Space Telescope. The observations were taken in August 2003. The top row reveals Uranus and Neptune in natural colors, showing the planets as they would appear if we could see them through a telescope. The images are made of exposures taken with filters sensitive to red, green, and blue light. In the bottom images, astronomers used different color filters to detect features we can't see. The photographs demonstrate that, by using certain types of color filters, astronomers can extract more information about a celestial object than our eyes normally can see. At first glance, the top row of images makes the planets appear like twins. But the bottom row reveals that Uranus and Neptune are two different worlds. Uranus's rotational axis, for example, is tilted almost 90 degrees to Neptune's axis. The south poles of Uranus and Neptune are at the left and bottom, respectively. Both are tilted slightly toward Earth. Uranus also displays more contrast between both hemispheres. This may be caused by its extreme seasons. Both planets display a banding structure of clouds and hazes aligned parallel to the equator. Additionally, a few discrete cloud features appear bright orange or red. The color is due to methane absorption in the red part of the spectrum. Methane is third in abundance in the atmospheres of Uranus and Neptune after hydrogen and helium, which are both transparent. Colors in the bands correspond to variations in the altitude and thickness of hazes and clouds. The colors allow scientists to measure the altitudes of clouds from far away. Technical facts about this news release: About the Object Object Name: Uranus; Neptune Object Description: Planets Distance: The semi-major axis of Uranus's orbit about the sun is 19.18 Astronomical Units (A.U.) or roughly 2.9 billion km. The semi-major axis of Neptune's orbit about the Sun is 30.06 Astronomical Units (A.U.) or roughly 4.5 billion km. Dimensions: Uranus (without rings) has a diameter of roughly 32,000 miles (51,000 km) at the equator.Neptune has a diameter of roughly 30,800 miles (49,600 km) at the equator. About the Data Object: Uranus Uranus Neptune Instrument: ACS/HRC STIS/CCD STIS/CCD HST Programs: 9725: E. Karkoschka and M. Tomasko (U. AZ) 9035: E. Karkoschka (U. AZ), M. Lemmon (Texas A&M), M. Tomasko (U. AZ) 9330: E. Karkoschka (U. AZ), M. Lemmon (Texas A&M), M. Tomasko (U. AZ) Exposure Date(s): August 30, 2003 August 19, 2002 August 3, 2003 Filters: F435W, F550M, F658N, F660N, F775W, F814W, F850LP, and F892N G430L and G750L G430L, G750L, CLEAR, and F28X50LP "Note:" Uranus images within this press release were taken with ACS/HRC. They were color calibrated using STIS/CCD data of Uranus. Neptune images within this press release were taken with STIS/CCD. About the Image Image Credit: NASA and E. Karkoschka (University of Arizona) Release Date: January 22, 2004 Orientation: Rings and Moons Circling Uranus [ http://imgsrc.hubblesite.org/hu/db/2004/05/images/a/formats/compass_large_web.jpg ] Neptune as Seen with Color Filters [ http://imgsrc.hubblesite.org/hu/db/2004/05/images/b/formats/compass_large_web.jpg ] *News Release Number:*: STScI-2004-05c

*Description*: Atmospheric features on Uranus and Neptune are revealed in images taken with the Space Telescope Imaging Spectrograph and the Advanced Camera for Surveys aboard NASA's Hubble Space Telescope. The observations were taken in August 2003. The top row reveals Uranus and Neptune in natural colors, showing the planets as they would appear if we could see them through a telescope. The images are made of exposures taken with filters sensitive to red, green, and blue light. In the bottom images, astronomers used different color filters to detect features we can't see. The photographs demonstrate that, by using certain types of color filters, astronomers can extract more information about a celestial object than our eyes normally can see. At first glance, the top row of images makes the planets appear like twins. But the bottom row reveals that Uranus and Neptune are two different worlds. Uranus's rotational axis, for example, is tilted almost 90 degrees to Neptune's axis. The south poles of Uranus and Neptune are at the left and bottom, respectively. Both are tilted slightly toward Earth. Uranus also displays more contrast between both hemispheres. This may be caused by its extreme seasons. Both planets display a banding structure of clouds and hazes aligned parallel to the equator. Additionally, a few discrete cloud features appear bright orange or red. The color is due to methane absorption in the red part of the spectrum. Methane is third in abundance in the atmospheres of Uranus and Neptune after hydrogen and helium, which are both transparent. Colors in the bands correspond to variations in the altitude and thickness of hazes and clouds. The colors allow scientists to measure the altitudes of clouds from far away. Technical facts about this news release: About the Object Object Name: Uranus; Neptune Object Description: Planets Distance: The semi-major axis of Uranus's orbit about the sun is 19.18 Astronomical Units (A.U.) or roughly 2.9 billion km. The semi-major axis of Neptune's orbit about the Sun is 30.06 Astronomical Units (A.U.) or roughly 4.5 billion km. Dimensions: Uranus (without rings) has a diameter of roughly 32,000 miles (51,000 km) at the equator.Neptune has a diameter of roughly 30,800 miles (49,600 km) at the equator. About the Data Object: Uranus Uranus Neptune Instrument: ACS/HRC STIS/CCD STIS/CCD HST Programs: 9725: E. Karkoschka and M. Tomasko (U. AZ) 9035: E. Karkoschka (U. AZ), M. Lemmon (Texas A&M), M. Tomasko (U. AZ) 9330: E. Karkoschka (U. AZ), M. Lemmon (Texas A&M), M. Tomasko (U. AZ) Exposure Date(s): August 30, 2003 August 19, 2002 August 3, 2003 Filters: F435W, F550M, F658N, F660N, F775W, F814W, F850LP, and F892N G430L and G750L G430L, G750L, CLEAR, and F28X50LP "Note:" Uranus images within this press release were taken with ACS/HRC. They were color calibrated using STIS/CCD data of Uranus. Neptune images within this press release were taken with STIS/CCD. About the Image Image Credit: NASA and E. Karkoschka (University of Arizona) Release Date: January 22, 2004 Orientation: Rings and Moons Circling Uranus [ http://imgsrc.hubblesite.org/hu/db/2004/05/images/a/formats/compass_large_web.jpg ] Neptune as Seen with Color Filters [ http://imgsrc.hubblesite.org/hu/db/2004/05/images/b/formats/compass_large_web.jpg ] *News Release Number:*: STScI-2004-05c

*Description*: Atmospheric features on Uranus and Neptune are revealed in images taken with the Space Telescope Imaging Spectrograph and the Advanced Camera for Surveys aboard NASA's Hubble Space Telescope. The observations were taken in August 2003. The top row reveals Uranus and Neptune in natural colors, showing the planets as they would appear if we could see them through a telescope. The images are made of exposures taken with filters sensitive to red, green, and blue light. In the bottom images, astronomers used different color filters to detect features we can't see. The photographs demonstrate that, by using certain types of color filters, astronomers can extract more information about a celestial object than our eyes normally can see. At first glance, the top row of images makes the planets appear like twins. But the bottom row reveals that Uranus and Neptune are two different worlds. Uranus's rotational axis, for example, is tilted almost 90 degrees to Neptune's axis. The south poles of Uranus and Neptune are at the left and bottom, respectively. Both are tilted slightly toward Earth. Uranus also displays more contrast between both hemispheres. This may be caused by its extreme seasons. Both planets display a banding structure of clouds and hazes aligned parallel to the equator. Additionally, a few discrete cloud features appear bright orange or red. The color is due to methane absorption in the red part of the spectrum. Methane is third in abundance in the atmospheres of Uranus and Neptune after hydrogen and helium, which are both transparent. Colors in the bands correspond to variations in the altitude and thickness of hazes and clouds. The colors allow scientists to measure the altitudes of clouds from far away. Technical facts about this news release: About the Object Object Name: Uranus; Neptune Object Description: Planets Distance: The semi-major axis of Uranus's orbit about the sun is 19.18 Astronomical Units (A.U.) or roughly 2.9 billion km. The semi-major axis of Neptune's orbit about the Sun is 30.06 Astronomical Units (A.U.) or roughly 4.5 billion km. Dimensions: Uranus (without rings) has a diameter of roughly 32,000 miles (51,000 km) at the equator.Neptune has a diameter of roughly 30,800 miles (49,600 km) at the equator. About the Data Object: Uranus Uranus Neptune Instrument: ACS/HRC STIS/CCD STIS/CCD HST Programs: 9725: E. Karkoschka and M. Tomasko (U. AZ) 9035: E. Karkoschka (U. AZ), M. Lemmon (Texas A&M), M. Tomasko (U. AZ) 9330: E. Karkoschka (U. AZ), M. Lemmon (Texas A&M), M. Tomasko (U. AZ) Exposure Date(s): August 30, 2003 August 19, 2002 August 3, 2003 Filters: F435W, F550M, F658N, F660N, F775W, F814W, F850LP, and F892N G430L and G750L G430L, G750L, CLEAR, and F28X50LP "Note:" Uranus images within this press release were taken with ACS/HRC. They were color calibrated using STIS/CCD data of Uranus. Neptune images within this press release were taken with STIS/CCD. About the Image Image Credit: NASA and E. Karkoschka (University of Arizona) Release Date: January 22, 2004 Orientation: Rings and Moons Circling Uranus [ http://imgsrc.hubblesite.org/hu/db/2004/05/images/a/formats/compass_large_web.jpg ] Neptune as Seen with Color Filters [ http://imgsrc.hubblesite.org/hu/db/2004/05/images/b/formats/compass_large_web.jpg ] *News Release Number:*: STScI-2004-05c

This represents the outer planets Jupiter, Saturn, Uranus and Neptune (alas, poor Pluto -- too small and too far out). The planets are to scale, and the orbits are also to scale although a different scale. The relative motion is produced by the ratios of the gears. See my posts ORRERY OF THE INNER PLANETS https://www.thingiverse.com/thing:3428770 and EARTH MOON TELLURION https://www.thingiverse.com/thing:2792105 for companion pieces. The video is at https://youtu.be/p71juy3I644. PLEASE NOTE that this is a very tricky print. All the parts must mesh precisely. Differences in slicers, printers and software may create very small variations that will require adjustments, filing, smoothing, and even wedging. Be prepared to adjust the model carefully.

Expands the Kerbol system with new planets and moons based on Saturn, Uranus, Neptune and their moons Homepage: http://forum.kerbalspaceprogram.com/threads/104280-0-90-Outer-Planet-Mods-Expands-the-Kerbol-system-with-new-planets-based-on-Saturn License(s): CC-BY-NC-SA-4.0

Technical facts about this news release: About the Object Object Name: Uranus; Neptune Object Description: Planets Distance: The semi-major axis of Uranus's orbit about the sun is 19.18 Astronomical Units (A.U.) or roughly 2.9 billion km. The semi-major axis of Neptune's orbit about the Sun is 30.06 Astronomical Units (A.U.) or roughly 4.5 billion km. Dimensions: Uranus (without rings) has a diameter of roughly 32,000 miles (51,000 km) at the equator.Neptune has a diameter of roughly 30,800 miles (49,600 km) at the equator. About the Data Object: Uranus Uranus Neptune Instrument: ACS/HRC STIS/CCD STIS/CCD HST Programs: 9725: E. Karkoschka and M. Tomasko (U. AZ) 9035: E. Karkoschka (U. AZ), M. Lemmon (Texas A&M), M. Tomasko (U. AZ) 9330: E. Karkoschka (U. AZ), M. Lemmon (Texas A&M), M. Tomasko (U. AZ) Exposure Date(s): August 30, 2003 August 19, 2002 August 3, 2003 Filters: F435W, F550M, F658N, F660N, F775W, F814W, F850LP, and F892N G430L and G750L G430L, G750L, CLEAR, and F28X50LP "Note:" Uranus images within this press release were taken with ACS/HRC. They were color calibrated using STIS/CCD data of Uranus. Neptune images within this press release were taken with STIS/CCD. About the Image Image Credit: NASA and E. Karkoschka (University of Arizona) Release Date: January 22, 2004 Orientation: Rings and Moons Circling Uranus [ http://imgsrc.hubblesite.org/hu/db/2004/05/images/a/formats/compass_large_web.jpg ] Neptune as Seen with Color Filters [ http://imgsrc.hubblesite.org/hu/db/2004/05/images/b/formats/compass_large_web.jpg ] *News Release Number:*: STScI-2004-05f

In the last year we have continued our program of near infrared imaging of the outer planets of the solar system. Uranus is virtually invisible at 2.3 microns, showing that the methane is an effective absorber of the incident sunlight and that there is very little aerosol content in the upper atmosphere. On the other hand, Neptune shows a haze present over the entire Northern Hemisphere at 2.3 microns. This leads to the inference that there is an aerosol layer at a high altitude. We have recovered the Neptune satellite, 1989 N1, which was first discovered in Voyager images. The satellite is exceedingly faint in the near infrared, and was detectable only because the planet itself was comparatively faint at this wavelength. Observations of this satellite, coupled with the Voyager images, permit us to substantially refine the satellite's orbit, and hence carefully probe the gravitational field of Neptune.

Scaling laws for possible outer planet magnetospheres are derived. These suggest that convection and its associated auroral effects will play a relatively smaller role than at earth, and that there is a possibility that they could have significant radiation belts of energetic trapped particles.