Venera Landers
Don S. Montgomery, US Navy (Ret.). Public domain (US government work).
Overview
Section titled “Overview”A machine that lands on Venus is not exploring an environment so much as racing it. At the surface, temperature runs near 460 C and pressure near 90 bar, conditions under which aluminum and most conventional electronics simply stop functioning [7]. No structure built of ordinary materials survives there indefinitely, so every Venera and VeGa lander was designed around a clock rather than a service life: how long the interior stayed cool enough to work before it equalized with the outside.
The Venera and VeGa landers are the only machines that have ever operated on the surface of Venus. Venera 7 made the first successful soft landing there on 15 December 1970, returning a single telemetered surface temperature of 747 K before its transmitter went silent [1]. Venera 9 and 10 followed in 1975, returning the first images from the surface of another planet and running for 53 and 65 minutes with the interior still below 60 C when contact ended [2]. Across the Venera and VeGa lander line, demonstrated electronics survival on the surface ranges from 23 to 127 minutes [5], and that range is the entire flight record of surface operation on Venus: it has not been extended since.
Design, and why it never diverged
Section titled “Design, and why it never diverged”The lander that could survive Venus at all was a sealed, thermally insulated pressure vessel, pre-chilled before atmospheric entry so the interior started the descent cold. Venera 9 and 10 were conditioned to between -8 and +10 C at separation from the flyby bus, entered at 10.7 km/s decelerating to 250 m/s, released their main parachutes at 65 km and jettisoned them at 50 km to fall the rest of the way on the aeroshell alone, reaching about 7 m/s at touchdown into a crushable, torus-shaped landing ring [2]. That profile, entry near 10 to 11 km/s, parachute jettison near 50 km and touchdown near 7 to 8 m/s, holds across the later Venera missions as well [4]. The descent through the dense lower atmosphere was deliberately fast, trading a harder landing for less time spent soaking up heat before the vessel reached the ground and started spending its cold reserve [2].
Every Venera and VeGa lander used that same pre-chilled sealed-vessel architecture; nothing else could be built and qualified for flight in the time available. The mission did not necessarily end when the electronics failed: Venera 9 and 10 stopped on an automatic command when the radio window to the flyby bus closed, with the interior still short of the survival limit [2]. That means the true thermal endurance of the design, as opposed to the time it happened to have a working relay, was never actually measured to its end on those two landers.
What the ground was actually like
Section titled “What the ground was actually like”Venera 9 and 10 measured 730 to 740 K and 88 to 94 atm at their landing sites, with surface wind of only 0.5 to 1 m/s measured a meter above the ground, both sites showing hard rock or slabs with a fine-grained matrix between them rather than deep regolith, and a gamma densitometer reading a bulk density of 2.8 plus or minus 0.1 g/cm3 for the hard material at the Venera 10 site [3]. That densitometer arm, striking the ground at 7 m/s under a 2 kg mass, left no visible mark at the Venera 10 site and only possibly cracked one boulder at Venera 9, the only in-situ mechanical strength data anyone has from the surface of Venus, and the most surprising result from either lander was optical rather than thermal: both carried floodlights because natural illumination under the cloud deck was expected to be low, and natural daylight completely overwhelmed the artificial sources at both sites, a design assumption the mission got backward [3].
What has changed since, and what it would enable
Section titled “What has changed since, and what it would enable”The Venera lifetime is a property of the vessel, not a hard limit set by Venus itself. Two lines of work since have targeted it directly.
The first is qualifying hardware against the actual atmospheric chemistry rather than against temperature and pressure alone. Reproducing temperature and pressure is explicitly insufficient to qualify parts for a prolonged surface mission [6], which is why the ground chamber built for this purpose carries nine independently mass-flow-controlled gas streams carrying SO2, COS, CO, H2O, HCl, NO and HF alongside the carbon dioxide and nitrogen, rather than a furnace and a plain pressure vessel [7]. Materials testing in that chamber found gold and bulk ceramics such as alumina, fused quartz, silicon carbide and silicon nitride showing no measurable change after 42 days at 92 bar and 467 C, while common steels and several nickel alloys grew double-layered oxide and sulfide scales in the same exposure [14].
The second is removing the requirement for a cooled interior altogether. Silicon carbide junction field effect transistor integrated circuits have run continuously at 500 C for 10,100 hours, 421 days, in air, with output parameters stable to within 5 percent after a 100- to 200-hour burn-in [10]. The failure mechanism at that temperature is not the semiconductor: it is thermal-stress cracking of the passivation stack over patterned metal topography, which admits oxygen to the interconnect below [9]. Under reproduced Venus chemistry rather than air, a packaged silicon carbide clock circuit has run for 60 days at 465 C and 90 bar [8]. A ten-chip lander sensor board built on that technology was tested unsheltered in the chamber and failed at only 107 C during heat-up, a fault traced to a wafer process defect from fabrication rather than to a limit of the device technology itself [11]. A concept study for a 13.56 kg uncooled surface station built on this electronics line targets one Venus day, about 120 Earth days, using natural convection and a sodium sulfur battery in place of a pressure vessel and active cooling [12].
Against 23 to 127 minutes, that target is a change of roughly three orders of magnitude in surface duration, from the same environment [5][12].
Derived data still in service
Section titled “Derived data still in service”No engineering description of the Venera or VeGa lander structure, pre-chilling system, imaging system, surface drill or bus relay has been published in the open literature; the one gross structural figure available is a mass comparison, in which the Venera and VeGa entry spheres were traded against Pioneer Venus aeroshells in a later mission study whose 700 kg vehicle is described as comparable in mass to a Venera lander [6]. What survives in active use is the derived atmospheric data set. Venera and Pioneer Venus probe measurements together form the Venus International Reference Atmosphere, which the current NASA Venus-GRAM engineering model still runs on, height- and latitude-dependent from 0 to 100 km and carrying mean zonal wind data only to 80 km before the model switches to extrapolation [13]. The underlying atmosphere data in that model has not been updated since 2005 [13].
What is not established
Section titled “What is not established”No source consulted here describes the actual Venera or VeGa lander hardware: mass, internal layout, the pre-chilling method, the drill and its sample transfer, and the flyby-bus relay link are all absent from the open literature, leaving the 700 kg-class mass comparison as the only structural figure available [6]. Both Venera 9 and 10 landed on the illuminated side at similar low elevations, so nothing in that record constrains the night side, higher latitudes, or higher elevation, and the competing explanations for the hard surface material at both sites are not resolved by the panorama and densitometer data alone [3]. Neither lander reached its true thermal limit, since both ended on a radio-window command rather than a failure, so the achievable endurance of that specific sealed-vessel design was never measured to its end [2]. On the successor side, the silicon carbide electronics that could remove the pressure-vessel requirement have been demonstrated only in small numbers of prototype chips under single test campaigns, with no lot statistics and no qualified part, and the one board tested under full Venus surface conditions failed from a fabrication defect rather than confirming any resolved understanding of long-term reliability [11].
Status
Section titled “Status”Complete. No lander has operated on the Venus surface since the VeGa missions.
References
- Avduevsky, V. S., Marov, M. Y., Rozhdestvensky, M. K., Borodin, N. F. and Kerzhanovich, V. V. (1971). Soft Landing of Venera 7 on the Venus Surface and Preliminary Results of Investigations of the Venus Atmosphere
. Journal of the Atmospheric Sciences, 2. Source
BibTeX
@article{avduevsky1971soft, title = {Soft Landing of Venera 7 on the Venus Surface and Preliminary Results of Investigations of the Venus Atmosphere}, author = {Avduevsky, V. S. and Marov, M. Ya. and Rozhdestvensky, M. K. and Borodin, N. F. and Kerzhanovich, V. V.}, journal = {Journal of the Atmospheric Sciences}, volume = {28}, number = {2}, pages = {263-269}, year = {1971}, doi = {10.1175/1520-0469(1971)028<0263:slovot>2.0.co;2}, abstract = {A soft landing on the planet Venus was successfully accomplished by the automatic interplanetary station Venera 7. The temperature of the Venus atmosphere was measured during the descent and at the surface after landing. The variation of temperature and pressure with altitude on Venus was determined down to the surface by combining the temperature measurements with descent velocity derived from the Doppler shift data during the descent, and by considering the data collected previously during the flights of Veneras 4, 5 and 6.} } - Keldysh, M. V. (1977). Venus Exploration with the Venera 9 and Venera 10 Spacecraft
. Icarus, 4. Source
BibTeX
@article{keldysh1977venus, title = {{Venus} Exploration with the {Venera} 9 and {Venera} 10 Spacecraft}, author = {Keldysh, M. V.}, journal = {Icarus}, volume = {30}, number = {4}, pages = {605--625}, year = {1977}, doi = {10.1016/0019-1035(77)90085-9} } - Florensky, C. P., Ronca, L. B., Basilevsky, A. T., Burba, G. A., Nikolaeva, O. V., Pronin, A. A., Trakhtman, A. M., Volkov, V. P. and Zazetsky, V. V. (1977). The Surface of Venus as Revealed by Soviet Venera 9 and 10
. Geological Society of America Bulletin, 11. Source
BibTeX
@article{florensky1977surface, title = {The Surface of {Venus} as Revealed by {Soviet} {Venera} 9 and 10}, author = {Florensky, C. P. and Ronca, L. B. and Basilevsky, Alexander T. and Burba, G. A. and Nikolaeva, O. V. and Pronin, A. A. and Trakhtman, A. M. and Volkov, V. P. and Zazetsky, V. V.}, journal = {Geological Society of America Bulletin}, volume = {88}, number = {11}, pages = {1537--1545}, year = {1977}, doi = {10.1130/0016-7606(1977)88<1537:tsovar>2.0.co;2}, abstract = {Research Article| November 01, 1977 The surface of Venus as revealed by Soviet Venera 9 and 10 C. P. FLORENSKY; C. P. FLORENSKY 1V. I. Vernadsky Institute of Geochemistry and Analytical Chemistry, Academy of Sciences of the USSR, 47-a Vorobjovskoe Shosse, Moscow 117334, USSR Search for other works by this author on: GSW Google Scholar L. B. RONCA; L. B. RONCA 1V. I. Vernadsky Institute of Geochemistry and Analytical Chemistry, Academy of Sciences of the USSR, 47-a Vorobjovskoe Shosse, Moscow 117334, USSR Search for other works by this author on: GSW Google Scholar A. T. BASILEVSKY; A. T. BASILEVSKY 1V. I. Vernadsky Institute of Geochemistry and Analytical Chemistry, Academy of Sciences of the USSR, 47-a Vorobjovskoe Shosse, Moscow 117334, USSR Search for other works by this author on: GSW Google Scholar G. A. BURBA; G. A. BURBA 1V. I. Vernadsky Institute of Geochemistry and Analytical Chemistry, Academy of Sciences of the USSR, 47-a Vorobjovskoe Shosse, Moscow 117334, USSR Search for other works by this author on: GSW Google Scholar O. V. NIKOLAEVA; O. V. NIKOLAEVA 1V. I. Vernadsky Institute of Geochemistry and Analytical Chemistry, Academy of Sciences of the USSR, 47-a Vorobjovskoe Shosse, Moscow 117334, USSR Search for other works by this author on: GSW Google Scholar A. A. PRONIN; A. A. PRONIN 1V. I. Vernadsky Institute of Geochemistry and Analytical Chemistry, Academy of Sciences of the USSR, 47-a Vorobjovskoe Shosse, Moscow 117334, USSR Search for other works by this author on: GSW Google Scholar A. M. TRAKHTMAN; A. M. TRAKHTMAN 1V. I. Vernadsky Institute of Geochemistry and Analytical Chemistry, Academy of Sciences of the USSR, 47-a Vorobjovskoe Shosse, Moscow 117334, USSR Search for other works by this author on: GSW Google Scholar V. P. VOLKOV; V. P. VOLKOV 1V. I. Vernadsky Institute of Geochemistry and Analytical Chemistry, Academy of Sciences of the USSR, 47-a Vorobjovskoe Shosse, Moscow 117334, USSR Search for other works by this author on: GSW Google Scholar V. V. ZAZETSKY V. V. ZAZETSKY 1V. I. Vernadsky Institute of Geochemistry and Analytical Chemistry, Academy of Sciences of the USSR, 47-a Vorobjovskoe Shosse, Moscow 117334, USSR Search for other works by this author on: GSW Google Scholar Author and Article Information C. P. FLORENSKY 1V. I. Vernadsky Institute of Geochemistry and Analytical Chemistry, Academy of Sciences of the USSR, 47-a Vorobjovskoe Shosse, Moscow 117334, USSR L. B. RONCA 1V. I. Vernadsky Institute of Geochemistry and Analytical Chemistry, Academy of Sciences of the USSR, 47-a Vorobjovskoe Shosse, Moscow 117334, USSR A. T. BASILEVSKY 1V. I. Vernadsky Institute of Geochemistry and Analytical Chemistry, Academy of Sciences of the USSR, 47-a Vorobjovskoe Shosse, Moscow 117334, USSR G. A. BURBA 1V. I. Vernadsky Institute of Geochemistry and Analytical Chemistry, Academy of Sciences of the USSR, 47-a Vorobjovskoe Shosse, Moscow 117334, USSR O. V. NIKOLAEVA 1V. I. Vernadsky Institute of Geochemistry and Analytical Chemistry, Academy of Sciences of the USSR, 47-a Vorobjovskoe Shosse, Moscow 117334, USSR A. A. PRONIN 1V. I. Vernadsky Institute of Geochemistry and Analytical Chemistry, Academy of Sciences of the USSR, 47-a Vorobjovskoe Shosse, Moscow 117334, USSR A. M. TRAKHTMAN 1V. I. Vernadsky Institute of Geochemistry and Analytical Chemistry, Academy of Sciences of the USSR, 47-a Vorobjovskoe Shosse, Moscow 117334, USSR V. P. VOLKOV 1V. I. Vernadsky Institute of Geochemistry and Analytical Chemistry, Academy of Sciences of the USSR, 47-a Vorobjovskoe Shosse, Moscow 117334, USSR V. V. ZAZETSKY 1V. I. Vernadsky Institute of Geochemistry and Analytical Chemistry, Academy of Sciences of the USSR, 47-a Vorobjovskoe Shosse, Moscow 117334, USSR Publisher: Geological Society of America First Online: 01 Jun 2017 Online ISSN: 1943-2674 Print ISSN: 0016-7606 Geological Society of America GSA Bulletin (1977) 88 (11): 1537–1545. https://doi.org/10.1130/0016-7606(1977)88<1537:TSOVAR>2.0.CO;2 Article history First Online: 01 Jun 2017 Cite View This Citation Add to Citation Manager Share Icon Share Facebook Twitter LinkedIn MailTo Tools Icon Tools Get Permissions Search Site Citation C. P. FLORENSKY, L. B. RONCA, A. T. BASILEVSKY, G. A. BURBA, O. V. NIKOLAEVA, A. A. PRONIN, A. M. TRAKHTMAN, V. P. VOLKOV, V. V. ZAZETSKY; The surface of Venus as revealed by Soviet Venera 9 and 10. GSA Bulletin 1977;; 88 (11): 1537–1545. doi: https://doi.org/10.1130/0016-7606(1977)88<1537:TSOVAR>2.0.CO;2 Download citation file: Ris (Zotero) Refmanager EasyBib Bookends Mendeley Papers EndNote RefWorks BibTex toolbar search Search Dropdown Menu toolbar search search input Search input auto suggest filter your search All ContentBy SocietyGSA Bulletin Search Advanced Search Abstract The soft landers Venera 9 and 10 transmitted information to Earth about conditions on the surface of Venus. Temperature measurements in both locations ranged from 730° to 740°K, and pressure measurements ranged from 88 to 94 atm. Wind velocities were 0.5 to 1 m/sec. The radioactive content of material below the spacecraft was similar to that of Earth's basalt. The hardness of some of the formations was estimated to be comparable to Earth's hard rocks. The density of a hard formation was measured by Venera 10 to be 2.8 ± 0.1 g/cm3.Panoramic television cameras provided photographs of the landing areas. The types of computer enhancements to which the photographs were subjected are briefly discussed.Venera 9 landed on a slope composed of slabs and a fine-grained matrix; Venera 10 landed on a plain composed of scattered outcrops separated by a fine-grained matrix. Detailed descriptions of the landing areas are presented.The available chemical and dynamic information about the conditions at the surface of the planet indicates that the atmosphere has a high efficiency in lifting and transporting loose small particles but that very little ablation of hard material is to be expected.Assuming thermodynamic equilibrium between atmosphere and surface materials, solid-gas interaction may occur and produce some disintegration of hard rocks and (or) some lithification of loose material, respectively by the increase in volume of newly formed minerals and by the formation of films or crusts. A vertical thermal gradient and vertical movements of gases or rocks are necessary. It is concluded, however, that the scale of chemical changes may be limited.The photographs show that at least two types of geomorphic degradation occur. The slabs of Venera 9 appear to be mass wasting downhill, and the outcrops of Venera 10 show evidence of rounding of corners and smoothing of surfaces. The mass wasting is likely to be caused by gravity and perhaps activated by quakes or other geologic processes. The rounding and smoothing processes are probably due to some atmospheric action.Six possible origins of the slabs and outcrops are discussed: (1) surface lava extrusion, (2) igneous intrusion later exposed by erosion, (3) pyroclastic fall, (4) impact lithification, (5) sedimentary rock lithified at depth and later exposed by erosion, and (6) lithification (or metamorphism) of loose material by atmospheric action at the surface.A model of the surface geology of Venus is presented in which fine material is gently moved by Venusian winds. Hard material is occasionally formed at the surface, either by lithification through atmospheric processes or by volcanic falls. Removal of loose material by winds will cause some of the lithified units to stand out as positive relief features and be subjected to rounding of corners and smoothing of surfaces. If a slope exists, the lithified units will break into slabs and mass waste downhill. First Page Preview Close Modal You do not have access to this content, please speak to your institutional administrator if you feel you should have access.} } - Mischna, M. (2025). The Science of Entry, Descent, and Landing in the Venus, Jupiter, and Saturn Systems
. Oxford Research Encyclopedia of Planetary Science. Source
BibTeX
@inproceedings{mischna2025science, title = {The Science of Entry, Descent, and Landing in the Venus, Jupiter, and Saturn Systems}, author = {Mischna, Michael}, booktitle = {Oxford Research Encyclopedia of Planetary Science}, publisher = {JPL Open Repository}, year = {2025}, doi = {10.48577/jpl.plm2tj} } - Sauder, J., Hilgemann, E., Bienstock, B. and Parness, A. (2017). An Automaton Rover Enabling Long Duration In-Situ Science in Extreme Environments
. IEEE Aerospace Conference. Source
BibTeX
@inproceedings{sauder2017automatona, title = {An Automaton Rover Enabling Long Duration In-Situ Science in Extreme Environments}, author = {Sauder, Jonathan and Hilgemann, Evan and Bienstock, Bernard and Parness, Aaron}, booktitle = {IEEE Aerospace Conference}, pages = {1-10}, publisher = {IEEE}, year = {2017}, doi = {10.1109/aero.2017.7943829} } - Sauder, J., Hilgemann, E., Johnson, M., Parness, A., Bienstock, B., Hall, J., Kawata, J. and Stack, K. (2017). Automaton Rover for Extreme Environments
. NASA Jet Propulsion Laboratory, 20170002798. Source
BibTeX
@techreport{sauder2017automaton, title = {Automaton Rover for Extreme Environments}, author = {Sauder, Jonathan and Hilgemann, Evan and Johnson, Michael and Parness, Aaron and Bienstock, Bernie and Hall, Jeffery and Kawata, Jessie and Stack, Kathryn}, number = {20170002798}, institution = {NASA Jet Propulsion Laboratory}, year = {2017}, url = {https://ntrs.nasa.gov/citations/20170002798}, abstract = {Almost 2,300 years ago the ancient Greeks built the Antikythera automaton. This purely mechanical computer accurately predicted past and future astronomical events long before electronics existed1. Automata have been credibly used for hundreds of years as computers, art pieces, and clocks. However, in the past several decades automata have become less popular as the capabilities of electronics increased, leaving them an unexplored solution for robotic spacecraft. The Automaton Rover for Extreme Environments (AREE) proposes an exciting paradigm shift from electronics to a fully mechanical system, enabling longitudinal exploration of the most extreme environments within the solar system. } } - Kremic, T., Vento, D., Lalli, N. and Palinski, T. (2014). Extreme Environment Simulation - Current and New Capabilities to Simulate Venus and Other Planetary Bodies
. IEEE Aerospace Conference, 20140013390. Source
BibTeX
@inproceedings{kremic2014extreme, title = {Extreme Environment Simulation - Current and New Capabilities to Simulate Venus and Other Planetary Bodies}, author = {Kremic, Tibor and Vento, Dan and Lalli, Nick and Palinski, Timothy}, booktitle = {IEEE Aerospace Conference}, number = {20140013390}, pages = {1-9}, institution = {NASA}, year = {2014}, doi = {10.1109/aero.2014.6836350}, abstract = {Science, technology, and planetary mission communities have a growing interest in components and systems that are capable of working in extreme (high) temperature and pressure conditions. Terrestrial applications range from scientific research, aerospace, defense, automotive systems, energy storage and power distribution, deep mining and others. As the target environments get increasingly extreme, capabilities to develop and test the sensors and systems designed to operate in such environments will be required. An application of particular importance to the planetary science community is the ability for a robotic lander to survive on the Venus surface where pressures are nearly 100 times that of Earth and temperatures approach 500C. The scientific importance and relevance of Venus missions are stated in the current Planetary Decadal Survey. Further, several missions to Venus were proposed in the most recent Discovery call. Despite this interest, the ability to accurately simulate Venus conditions at a scale that can test and validate instruments and spacecraft systems and accurately simulate the Venus atmosphere has been lacking. This paper discusses and compares the capabilities that are known to exist within and outside the United States to simulate the extreme environmental conditions found in terrestrial or planetary surfaces including the Venus atmosphere and surface. The paper then focuses on discussing the recent additional capability found in the NASA Glenn Extreme Environment Rig (GEER). The GEER, located at the NASA Glenn Research Center in Cleveland, Ohio, is designed to simulate not only the temperature and pressure extremes described, but can also accurately reproduce the atmospheric compositions of bodies in the solar system including those with acidic and hazardous elements. GEER capabilities and characteristics are described along with operational considerations relevant to potential users. The paper presents initial operating results and concludes with a sampling of investigations or tests that have been requested or expected.} } - Chen, L.-Y., Neudeck, P. G., Meredith, R. D., Lukco, D., Spry, D. J., Nakley, L. M., Phillips, K. G., Beheim, G. M. and Hunter, G. W. (2018). Sixty Earth-Days Test of a Prototype Pt/HTCC Alumina Package in Simulated Venus Environment
. Additional Conferences, 20180006758. Source
BibTeX
@inproceedings{chen2018sixty, title = {Sixty Earth-Days Test of a Prototype Pt/HTCC Alumina Package in Simulated Venus Environment}, author = {Chen, Liang-Yu and Neudeck, Philip G. and Meredith, Roger D. and Lukco, Dorothy and Spry, David J. and Nakley, Leah M. and Phillips, Kyle G. and Beheim, Glenn M. and Hunter, Gary W.}, booktitle = {Additional Conferences}, volume = {2018}, number = {20180006758}, pages = {000015-000021}, institution = {NASA}, address = {Albuquerque, New Mexico}, year = {2018}, doi = {10.4071/2380-4491-2018-hiten-0000015}, abstract = {Abstract This paper presents experimental results of a prototype high temperature co-fired ceramic (HTCC) package with Au/Pt metallization in a three-phase harsh environment test that culminated with 60-day demonstration in simulated Venus surface environment of 465 °C with corrosive atmosphere at 90 bar pressure. The prototype package is based on previously developed and reported HTCC package successfully tested with multiple analog and digital silicon carbide (SiC) high temperatures semiconductor integrated circuits (ICs) at NASA Glenn Research Center in 500 °C Earth air ambient for over ten thousands hours, and short-term tested at temperatures above 800 °C. The three-phase harsh environment test started with 48 hours in 465 °C Earth air, followed by 48 hours in 465 °C nitrogen at 90 bar pressure and 1400 hours in simulated Venus surface environment of 465 °C with corrosive atmosphere at 90 bar. Initial analytical results of the package materials and surfaces after exposure to Venus environment are discussed to assess the stability of the packaging materials in the tested environments. The test in simulated Venus environment was implemented in the NASA Glenn Extreme Environment Rig (GEER). The results of this study suggest that an effective encapsulation of areas of surface metallization and vicinities may help to improve electrical performance of a HTCC alumina packaging system in Venus environment.} } - Neudeck, P. G., Spry, D. J., Chen, L., Lukco, D., Chang, C. W. and Beheim, G. M. (2017). Experimentally Observed Electrical Durability of 4H-SiC JFET ICs Operating from 500 C to 700 C
. Materials Science Forum. Source
BibTeX
@inproceedings{neudeck2017experimentally, title = {Experimentally Observed Electrical Durability of 4H-SiC JFET ICs Operating from 500 C to 700 C}, author = {Neudeck, Philip G. and Spry, David J. and Chen, Liangyu and Lukco, Dorothy and Chang, Carl W. and Beheim, Glenn M.}, booktitle = {Materials Science Forum}, volume = {897}, pages = {567-570}, year = {2017}, doi = {10.4028/www.scientific.net/msf.897.567}, abstract = {Prolonged 500 °C to 700 °C electrical testing data from 4H-SiC junction field effect transistor (JFET) integrated circuits (ICs) are combined with post-testing microscopic studies in order to gain more comprehensive understanding of the durability limits of the present version of NASA Glenn's extreme temperature microelectronics technology. The results of this study support the hypothesis that T ≥ 500 °C durability-limiting IC failure initiates with thermal stress-related crack formation where dielectric passivation layers overcoat micron-scale vertical features including patterned metal traces.} } - Neudeck, P. G., Spry, D. J., Krasowski, M. J., Prokop, N. F., Beheim, G. M., Chen, L.-Y. and Chang, C. W. (2018). Yearlong 500 C Operational Demonstration of Up-scaled 4H-SiC JFET Integrated Circuits
. Additional Conferences. Source
BibTeX
@inproceedings{neudeck2018yearlong, title = {Yearlong 500 C Operational Demonstration of Up-scaled 4H-SiC JFET Integrated Circuits}, author = {Neudeck, Philip G. and Spry, David J. and Krasowski, Michael J. and Prokop, Norman F. and Beheim, Glenn M. and Chen, Liang-Yu and Chang, Carl W.}, booktitle = {Additional Conferences}, volume = {2018}, pages = {000071-000078}, year = {2018}, doi = {10.4071/2380-4491-2018-hiten-000071}, abstract = {Abstract This work describes recent progress in the design, processing, and testing of significantly up-scaled 500 °C durable 4H-SiC junction field effect transistor (JFET) integrated circuit (IC) technology with two-level interconnect undergoing development at NASA Glenn Research Center. For the first time, stable electrical operation of semiconductor ICs for over one year at 500 °C in air atmosphere is reported. These groundbreaking durability results were attained on two-level interconnect JFET demonstration ICs with 175 or more transistors on each chip. This corresponds to a more than 7-fold increase in 500 °C-durable circuit complexity from the 24 transistor ring oscillator ICs reported at HiTEC 2016 [1]. These results advance the technology foundation for realizing long-term durable 500 °C ICs with increased functional capability for combustion engine sensing and control, planetary exploration, deep-well drilling monitoring, and other harsh-environment applications.} } - Neudeck, P. G., Chen, L., Greer, L. C., Spry, D. J., Prokop, N. F., Lukco, D., Krasowski, M. J. and Hunter, G. W. (2024). Venus Surface Environmental Chamber Test of SiC JFET-R Multi-Chip Circuit Board
. Solid State Phenomena. Source
BibTeX
@article{neudeck2024venus, title = {Venus Surface Environmental Chamber Test of SiC JFET-R Multi-Chip Circuit Board}, author = {Neudeck, Philip G. and Chen, Liangyu and Greer, Lawrence C. and Spry, David J. and Prokop, Norman F. and Lukco, Dorothy and Krasowski, Michael J. and Hunter, Gary W.}, journal = {Solid State Phenomena}, volume = {358}, pages = {7--12}, year = {2024}, doi = {10.4028/p-u3mieo}, abstract = {This paper describes a first attempt to build and operate a multi-chip prototype lander control and sensor signal digitization electronics circuit board comprised of ten NASA Glenn IC Generation 11 SiC JFET-R IC chips in 460 °C, 9.4 MPa harsh Venus surface conditions. The lander circuit ceased electrical operation prematurely at 107 °C as the Venus chamber heated up. Microscopic post-test inspections indicate that only one of the ten SiC chips on the board failed. Most of circuit-damaging cracks observed on the failed chip corresponded to micron-scale irregularly-shaped dielectric film hillock defects. The study of these defects suggests minor processing changes to eliminate this suspected root failure cause.} } - Hunter, G. W., Izenberg, N., Oleson, S. R., Newman, J. M., Gilmore, M., Jessup, K. L., Herrick, R., Balcerski, J., Colozza, A., Faller, B., Fincannon, J., Fittje, J., Gyekenyesi, J., Jones, R., Klefman, B., Landis, G., Martini, M., McCarty, S., Packard, T., Smith, D. and Turnbull, E. (2020). Compass Final Report: Venus Bridge Orbiter and Surface Study (V-BOSS)
. NASA Glenn Research Center, NASA/TP-2020-220152. Source
BibTeX
@techreport{hunter2020compass, title = {Compass Final Report: Venus Bridge Orbiter and Surface Study (V-BOSS)}, author = {Hunter, Gary W. and Izenberg, Noam and Oleson, Steven R. and Newman, J. M. and Gilmore, Martha and Jessup, Kandis Lea and Herrick, Robert and Balcerski, Jeffrey and Colozza, Anthony and Faller, Brent and Fincannon, James and Fittje, James and Gyekenyesi, John and Jones, Robert and Klefman, Brandon and Landis, Geoffrey and Martini, Michael and McCarty, Steven and Packard, Thomas and Smith, David and Turnbull, Elizabeth}, number = {NASA/TP-2020-220152}, institution = {NASA Glenn Research Center}, year = {2020}, url = {https://ntrs.nasa.gov/citations/20200013062}, abstract = {The Venus Bridge Orbiter and Surface Study (V-BOSS) Compass concurrent engineering design team study shows that new, high-priority Venus science can be achieved using a linked Orbiter + Surface Element (Lander) mission concept within a $200M cost cap with assumptions. This is feasible through optimizing investment in early technologies and platforms, such as the Long-Lived In-Situ Solar System Explorer (LLISSE), leveraging known and flight-ready technology, and the overall use of simple, small, robust systems in innovative approaches to Venus exploration. This architecture allows a range of science investigations through modification of Orbiter-Lander platforms in this study through choice of other instruments (often sensors), science themes, or operational modes. In particular, a fundamental strength of this approach is to provide science not available in other ways by using simplified architectures including rugged systems operable in-situ on the Venus surface. Such investigations would be pathfinders for more complex, and more expensive, future missions. Additionally, the results of this study can be used to further champion the need, value and return of early investment technology programs for the hard problem of in-situ investigations at Venus.} } - Justh, H. L., Dwyer Cianciolo, A. M. and Hoffman, J. (2021). Venus Global Reference Atmospheric Model (Venus-GRAM): User Guide
. NASA Marshall Space Flight Center, NASA/TM-20210022168. Source
BibTeX
@techreport{justh2021venus, title = {Venus Global Reference Atmospheric Model (Venus-GRAM): User Guide}, author = {Justh, Hilary L. and Dwyer Cianciolo, Alicia M. and Hoffman, J.}, number = {NASA/TM-20210022168}, institution = {NASA Marshall Space Flight Center}, year = {2021}, url = {https://ntrs.nasa.gov/citations/20210022168}, abstract = {This Technical Memorandum (TM) presents the Venus Global Reference Atmospheric Model (Venus-GRAM) and the updated features of the GRAMs. Venus-GRAM is an engineering-oriented atmospheric model that estimates mean values and statistical variations of atmospheric properties for Venus. This TM summarizes the atmospheric data model in Venus-GRAM and provides a guide for the user to obtain, set up, and run the code in various configurations. Additional details regarding the Venus-GRAM input and output files and how to interpret Venus-GRAM results are also provided.} } - Costa, G. C. C., Jacobson, N. S., Lukco, D., Hunter, G. W., Nakley, L., Radoman-Shaw, B. G. and Harvey, R. P. (2017). Chemical and Microstructural Changes in Metallic and Ceramic Materials Exposed to Venusian Surface Conditions
. NASA, NASA/TM-2017-219437. Source
BibTeX
@techreport{costa2017chemical, title = {Chemical and Microstructural Changes in Metallic and Ceramic Materials Exposed to Venusian Surface Conditions}, author = {Costa, Gustavo C. C. and Jacobson, Nathan S. and Lukco, Dorothy and Hunter, Gary W. and Nakley, Leah and Radoman-Shaw, Brandon G. and Harvey, Ralph P.}, number = {NASA/TM-2017-219437}, institution = {NASA}, year = {2017}, url = {https://ntrs.nasa.gov/citations/20170006025}, abstract = {The chemical and microstructural behavior of steels (304, 310, 316, and 1018), nickel-based alloys (beta-NiAl, G30, and 625), gold, coatings (4YSZ, SilcoNert(TradeMark) 1040 (SilcoTek Co.), Dursan(TradeMark) (SilcoTek Co.), and porcelain), and bulk ceramics (alpha-Al2O3, fused quartz, beta-SiC, and alpha-Si3N4) were probed after exposure to supercritical fluid with temperature, pressure, and composition mimicking the Venus lower atmosphere. Exposures were carried out in the Glenn Extreme Environments Rig (GEER) chamber with the Venusian gas mixture (96.5% CO2, 3.5% N2, 30 ppm H2O, 150 ppm SO2, 28 ppm CO, 15 ppm OCS, 3 ppm H2S, 0.5 ppm HCl, and 5 ppb HF) at 92 bar (1330 psi) and 467 C (873 F) for durations of 10 and 42 days. An additional 21-day exposure was done to stainless steel uncoated and coated with SilcoNert(TradeMark) and Dursan(TradeMark). Samples were characterized before and after the experiment by gravimetric analysis, X-ray diffraction, X-ray photoelectron and Auger electron spectroscopies, and cross section electron microscopy analysis. All steels exposed for 10 and 42 days formed double-layered scales consisting mainly of metal (Cr, Fe, Ni) oxides and sulfides showing different chemistry, microstructure, and crystalline phases. The alloys G30 and 625 formed double-layered scales consisting mainly of nickel sulfides. After 10 days, the beta-NiAl exhibited no detectable scale, suggesting only a very thin film was formed. The 304 and 316 stainless steels coated with 4YSZ that were exposed for 10 and 42 days exhibited no significant oxidation. Steel 1018 coated with 4YSZ exhibited a corrosion scale of iron and/or chromium oxide formed at the base of the alloy. The 304 steel coated with porcelain did not exhibit corrosion, although the coating exhibited recession. SilcoNert(TradeMark) exposed for 10 and 42 days exhibited recession, although no oxidation was found to occur at the base of the alloy. Stainless steel 316 coated with Dursan(TradeMark) exhibited corrosion at the base of the alloy. All ceramics tested showed no clear evidence of reaction. The weight-gain-per-area performance of the materials exposed in the GEER for 10 and 42 days are reported from the lowest to the highest weight gain per area as follows: gold did not exhibit any weight change; nickel-based alloys: beta- NiAl < G30 < 625; steels: 304 < 310 < 316 < 1018; ceramics: considering the experimental uncertainties, no weight change was observed for all ceramics of this work (alpha-Al2O3, Si3N4, SiC, and amorphous SiO2).} }