

Welcome to DavidARoffman.com. This site documents 10 years of research about Martian meteorology that I have conducted in conjunction with my father, Barry S. Roffman (Lieutenant, U.S. Coast Guard-Retired). It also summarizes what I have been able to learn about Breakthrough Propulsion Physics, and it explores some of the physics projects that I wrote about while earning my B.S. in space physics at Embry-Riddle Aeronautical University (Daytona Beach, Florida) and my Master’s and PhD in physics with a specialization in Computational Condensed Matter Theory at the University of Florida. If you have questions about any of our research please contact us at Davidaroffman@gmail.com or MarsCorrect@Gmail.com.
EXTENSIVE ROFFMAN INTERVIEW ABOUT MARS IN ENGLISH AND ITALIAN: My father and I were interviewed about Mars for 3 hours 42 minutes on September 3, 2017. The interview was conducted via Skype by Marco de Marco in Amsterdam, and simultaneously translated into Italian. You can view it at this link.
The Table of Contents for this site is here.
MAIN DOCUMENTS SUPPORTING OUR POSITION THAT ALL NASA MARS WEATHER DATA IS FLAWED:
OCTOBER 25, 2019: BASIC REPORT for MARS CORRECT – CRITIQUE OF ALL NASA MARS WEATHER DATA
ABSTRACT: We present evidence that NASA is seriously understating Martian air pressure. Our 10-year study critiques 2,561 sols (~7.2 terrestrial years, 3.94 Martian years) of highly problematic MSL Rover Environmental Monitoring Station (REMS) weather data, and offers an in depth audit of over 8,311 hourly Viking 1 and 2 weather reports. We discuss analysis of technical papers, NASA documents, and personal interviews of transducer designers. We troubleshoot pressures based on radio occultation/spectroscopy, and the previously accepted small pressure ranges that could be measured by Viking 1 and 2 (18 mbar), Pathfinder and Phoenix (12 mbar), and MSL (11.5 mbar - altered to 14 mbar in 2017). For MSL there were several pressures published from August 30 to September 5, 2012 that were from 737 mbar to 747 mbar – two orders of magnitude high – only to be retracted. We challenged many pressures and NASA revised them down. However there are two pressure sensors ranges listed on a CAD for Mars Pathfinder. We long thought the CAD listed two different sensors, but based on specifications of a new Tavis sensor for InSight that is like that on PathFinder, it appears that the transducer could toggle between two pressures ranges: 0-0.174 PSIA/12 mbar (Tavis Dash 2) and 0-15 PSIA/1,034 mbar (Tavis Dash 1). Further, for the MSL according to an Abstract to the American Geophysical Union for the Fall 2012 meeting, The Finnish Meteorological Institute (FMI) states of their MSL (and Phoenix) Vaisala transducers, “The pressure device measurement range is 0 – 1025 hPa in temperature range of -45°C – 55°C, but its calibration is optimized for the Martian pressure range of 4 – 12 hPa.” So while we first thought that of the five landers that had meteorological suites, none could measure Earth-like pressures, in fact, three landers were actually equipped to get the job. Further, all original 19 low UV values were removed when we asked about them, although they eventually restored 12 of them. REMS always-sunny opacity reports were contradicted by Mars Reconnaissance Orbiter photos. Why REMS Team data was so wrong is a matter of speculation, but we demonstrate that their weather data was regularly revised after they studied online critiques in working versions of this report. REMS even labelled all dust 2018 Global Dust Storm weather as sunny, although they did list the UV values then as all low.
Vikings and MSL showed consistent timing of daily pressure spikes which we link to how gas pressure in a sealed container would vary with Absolute temperature, to heating by radioisotope thermoelectric generators (RTGs), and to dust clots at air access tubes and dust filters. Pathfinder, Phoenix and MSL wind measurements failed. Phoenix and MSL pressure transducer design problems included confusion about dust filter location, and lack of information about nearby heat sources due to International Traffic and Arms Regulations (ITAR). NASA Ames could not replicate dust devils at 10 mbar. Rapidly filled MER Spirit tracks required wind speeds of 80 mph at the assumed low pressures. These winds were never recorded on Mars. Nor could NASA explain drifting Barchan sand dunes. Based on the above and dust devils on Arsia Mons to altitudes of 17 km above areoid (Martian equivalent of sea level), spiral storms with 10 km eye-walls above Arsia Mons and similar storms above Olympus Mons (over 21 km high), dust storm opacity at MER Opportunity blacking out the sun, snow that descends 1 to 2 km in only 5 or 10 minutes, excessive aero braking, liquid water running on the surface in numerous locations at Recurring Slope Lineae (RSL) and stratus clouds 13 km above areoid, we argue for an average pressure at areoid of ~511 mbar rather than the accepted 6.1 mbar. This pressure grows to 1,050 mbar in the Hellas Basin.
JULY 16, 2018: PowerPoint version of our Basic Report is found at Mars Correct? Mars is Wet!
TABLE OF CONTENTS FOR MARS CORRECT - CRITIQUE OF ALL NASA MARS WEATHER DATA (Updated 9/23/2018) | |
1 | |
1. INTRODUCTION | 2 |
1.1 Comparison of Martian and terrestrial dust devils | 3 |
1.1.1 Geographic Occurrences and the Greenhouse and Thermophoresis Effect | 3 |
1.1.2 Seasonal Occurrences and Electrical Properties | 4 |
1.1.3. Size and Shape | 4 |
1.1.4. Diurnal Formation Rate and Lifetime | 4 |
1.1.5 Wind Speeds | 4 |
1.1.6 Core Temperature Excursions | 4 |
1.1.7 Dust Particle Size – The Problem of Martian Dust <2 Microns and Wind Speeds | 4 |
1.1.8. Core Pressure Excursions | 5 |
1.2. NASA Ames Test of Martian Pressures and Dust Devils | 8 |
9 | |
2.1 Viking 2 and Gay-Lussac’s Law | 11 |
16 | |
2.3. Which Transducers Were Used? | 19 |
2.4. Issues Raised by the FMI | 20 |
2.5. DID ANY TAVIS OR VAISALA TRANSDUCERS PEG OUT AT THEIR MAXIMUM PRESSURES? | 26 |
2.5.1 How extraordinary was the (temporary) 1,149 Pa pressure spike of MSL Sol 370? | 27 |
2.5.2. The importance of gleaning data from identification of our web site readers | 27 |
2.5.3 Why is it so wrong to alter data to fit an expected curve? | 34 |
2.6 The Dust filter on Viking | 37 |
2.6.1. The issue of Viking pressure reports and digitization | 37 |
2.6.2. The issue of daily pressure spikes at consistent time-bins. | 38 |
2.7. MSL Weather Reporting Fiasco | 43 |
3. CAVES ON AND SPIRAL CLOUDS ABOVE ARSIA MONS AND OLYMPUS MONS ON MARS. | 46 |
4. THE ISSUES OF SNOW, WATER ICE, AND CARBON DIOXIDE ON MARS. | 48 |
48 | |
4.1.1. Ls of minimum pressure | 49 |
4.1.2. Ls of maximum pressure | 49 |
62 | |
5.1 Shifting Standards – The Relationship of the MOLA Topography of Mars to the Mean Atmospheric Pressure. | 64 |
68 | |
69 | |
7.1 Anemometer/Telltale Wind Speed Issues | 70 |
7.2 Martian Bedforms – Too Much Movement of Sand Dunes and Ripples for 6.1 mbar | 72 |
7.2.1 Issues Raised by the paper on Planet-wide sand motion on Mars by Bridges et al. (2012) | 72 |
78 | |
83 | |
90 | |
10.1 Mars Global Surveyor (MGS) | 90 |
10.2 Mars Reconnaissance Orbiter (MRO) | 91 |
91 | |
11.1 Pressures Claimed for the 2018 Global Dust Storm | 94 |
11.2 Brief Summary of 2018 Dust Storm Data | 104 |
11.3 Possibility of a Biological Factor in Lifting Dust | 104 |
11.3.1 Martian Dust Storm Seasons | 105 |
11.4 Martian Dust Storm Paths and Radioactive Areas | 105 |
106 | |
109 | |
13.1 Did NASA ever publicly back 20 mbar on Mars? | 109 |
13.2 Biology, Methane, and a Possible Hint of the Real Martian Air Pressure | 110 |
13.3 Recurring Slope Lineae (RSL), Perchlorates and Running Water on Mars | 115 |
13.3.1 Length of daylight where RSL are found | 115 |
13.3.2 Latitudes, times and temperatures for evidence of running water | 117 |
13.3.3 The role of perchlorates in RSL | 118 |
13.4 Other Water on Mars – the Frozen Sea at Utopia Planitia | 120 |
13.5 The High End of Pressure Estimates for Mars…. | 123 |
13.6. Pressure Drop as MSL Climbs Mt. Sharp vs. Scale Height Predictions. | 128 |
137 | |
140 | |
141 | |
15.2. Winter Ground Temperatures above freezing in MSL Year 2 | 149 |
15.3. Why the early winter ground temperatures are so important and possible life seen on Sol 1185 | 149 |
154 | |
15.5. MSL Diurnal Temperature Variations | 157 |
15.5.1. Why does the temperature fall more degrees at MSL in summer nights than winter nights? | 161 |
15.6. Probable Failure of the Ground Temperature Sensor or Personnel Issues? | 161 |
168 | |
15.6.2 Personnel Issues. | 168 |
15.6.3 Mixed messages about the range and sensitivity of pressure sensors sent to Mars. | 170 |
175 | |
15.7 Temperature, Pressure and Albedo | 176 |
180 | |
16.1 Solar Longitude for sols at MSL with very high and low ultraviolet radiation. | 182 |
191 | |
17.1 ESA gets smarter – Raises ExoMars orbit due to excessive density of Mars’s atmosphere | 194 |
18. CONCLUSIONS | 196 |
19. RECOMMENDATIONS | 203 |
20. ACKNOWLEDGEMENTS | 204 |
205 | |
21. REFERENCES | 211 |
ANNEXES AND APPENDICES TO MARS CORRECT - CRITIQUE OF ALL NASA MARS WEATHER DATA:
SECTION | TOPIC | PAGE |
Annex Abstract | Overview of data in the Annexes | A-1 |
ANNEX A | VIKING 1 MORNING PRESSURE AND TEMPERATURE CHANGES and Mars Time-Bin Clock. | A-2 to A-59 |
ANNEX A Appendix 1 | VL-1 pressures of .26 to .3 time-bins & .3 to .34 time-bins. Sols 1-116. | A-3 to A-22 |
Appendix 2 | VL-1 pressures of .26 to .3 time-bins & .3 and .34 time-bins. Sols 134-199. | A-23 to A-34 |
Appendix 3 | VL-1 pressures of .26 to .3 time-bins & .3 and .34 time-bins. Sols 200-219. | A-35 to A-38 |
Appendix 4 | VL-1 pressures of .26 to .3 time-bins & .3 and .34 time-bins. Sols 220-304 | A-39 to A-50 |
Appendix 5 | VL-1 pressures of .26 to .3 time-bins & .3 and .34 time-bins. Sols 305-334 | A-51 to A-55 |
Appendix 6 | VL-1 pressures of .26 to .3 time-bins & .3 and .34 time-bins. Sols 335-350 | A-56 to A-59 |
ANNEX B | B-1 to B-39 | |
Appendix 1 | VL-2 pressures of .26 to .3 time-bins & .3 and .34 time-bins. Sols 156-175 | B-2 to B-5 |
Appendix 2 | VL-2 pressures of .26 to .3 time-bins & .3 and .34 time-bins. Sols 176-199. | B-6 to B-10 |
Appendix 3 | VL-2 pressures of .26 to .3 time-bins & .3 and .34 time-bins. Sols 201-260. | B-11 to B-20 |
Appendix 4 |
VL-2 pressures of .26 to .3 time-bins & .3 and .34 time-bins. Sols 261-290. | B-21 to B-26 |
Appendix 5 | VL-2 pressures of .26 to .3 time-bins & .3 and .34 time-bins. Sols 291-305. | B-27 to B-30 |
Appendix 6 | VL-2 pressures of .26 to .3 time-bins & .3 and .34 time-bins. Sols 306-361 | B-31 to B-39 |
ANNEX C | C-1 to C-54 | |
ANNEX D | D-1 to D-171 | |
Appendix 1 | Viking 1 Sols 1 to 199 | D-3 to D-94 |
Appendix 2 | Viking 1 Sols 200 to 350 | D-95 to D-171 |
ANNEX E | Measured vs. Predicted Pressure Percent Differences for Viking-1 Time-bins 0.3 and 0.34 | E-1 to E-14 |
ANNEX F | F-1 to F-18 | |
Appendix 1 | Percent Difference Flow Chart for Viking 1 Sols 1 to 116 & 200 to 350 | F-5 to F-16 |
Appendix 2 | Histogram with temperatures at successful predictions per time-bins | F-17 to F-18 |
ANNEX G | G-1 to G-13 | |
ANNEX H | Calibration Effort for the Mars Pathfinder Tavis Pressure Transducer and IMP Windsock Experiment | H-1 to H-43 |
ANNEX I | Pressures Reported by the Rover Environmental Monitoring Station (REMS). | I-1 to I-28 |
Appendix 1 | Print Screen Record of Original REMS Team and Ashima Research MSL Weather Reports | I-12 to I-28 |
ANNEX J | Concessions by Ashima Research and How to Correctly Calculate Daylight Hours for MSL | J- 1to J-19 |
ANNEX K | REMS Team and Ashima Research Weather Reports from Sol 15 to Sol 299. | K-1 to K-34 |
ANNEX L | L-1 to L-10 | |
ANNEX M | M-1 to M-38 | |
ANNEX N | Weather Reports for MSL Year 2 Ls 151 to Ls 270 (late winter to end of spring), Sols 670 to 864 | N-1 to N-13 |
ANNEX O | Weather Reports for MSL Year 2 Ls 270 to Ls 0 (summer), Sols 865 to 1,020 | O-1 to O-11 |
ANNEX P | Weather Reports for MSL Year 2 Ls 0 to Ls 90 (autumn), Sols 1019 to 1,213 | P-1 to P-15 |
ANNEX Q | Weather Reports for MSL Year 2 to 3 Winter, Ls 90 to Ls 180 (Sols 1,213 to 1,392) | Q-1 to Q-18 |
ANNEX R | Weather Reports for MSL Year 3 Spring, Ls 180 to Ls 270 (Sols 1,392 to 1,534 | R-1 to R-37 |
ANNEX S | Source: Document: Two Martian Years of MSL High Air and Ground Temperatures. | S-1 to S41 |
ANNEX T | Source Document: Two Martian Years of MSL Low Air and Ground Temperatures. | T-1 to T-64 |
ANNEX U | Comparison of Ultraviolet Radiation and Pressures at Gale Crater, Mars for MSL Years 1 and 2 | U-1 to U-28 |
ANNEX V | Weather Reports for MSL Year 3 Summer, Ls 270 to Ls 0 (Sols 1,534 to 1,686. | V-1 to V-28 |
ANNEX W | Weather Reports for MSL Year 3 Fall, Ls 0 to 90 (Sols 1,687 to 1,881 | W -1 to W-24 |
ANNEX X | Weather Reports for MSL Year 3-4 Winter, Ls 90 to 180 (Sols 1,881to 2060 | X-1 to X-31 |
Table 1 - Record of all MSL weather data published by NASA with printscreens showing how the data was altered over time, often in response to suggestions or comments made on this site and at http://marscorrect.com. | ||
MARS SCIENCE LABORATORY DAILY WEATHER REPORTS | ||
MARS SCIENCE LAB SOLS and LINKS | SOLAR LONGITUDE (Ls) | SEASONS |
150 to 150 | 4 SEASONS: Note: JPL labels the first year of MSL on Mars as Year 0. We call it Year 1. Although we looked at revising everything we have on all web sites to conform with JPL, the number of changes required is too massive. When it doubt about the year check the sol number involved. Their Year 1 is our Year 2, their Year 2 is our Year 3. | |
151 to 270 | WINTER TO SUMMER YEAR 2 | |
270 to 0 (360) | SUMMER YEAR 2 | |
0 to 90 | FALL YEAR 2 | |
90 to 180 | WINTER YEAR 2-3 | |
180 to 270 | SPRING YEAR 3 | |
270 to 0 (360) | SUMMER YEAR 3 | |
0 to 90 | FALL YEAR 3 | |
1881 to 2020 | 90 to 180 | WINTER YEAR 3-4 |
2060 and onward | 180 to 270 | SPRING YEAR 4 |
COMPARISONS BETWEEN MSL YEAR 0 AND MSL YEAR 1 DATA FOR THE SAME LS | ||
Pressure and Ultraviolet Radiation | ||
High Air and Ground Temperatures for MSL | Note 1: Ground temperature sensor is only accurate to 10K. Note 2 dated February 5, 2016: There are unexpected ground temperatures at or above freezing for almost every sol for 3 weeks after the start of MSL Year 1's winter. | |
Low Air and Ground Temperatures for MSL | ||
Diurnal Air Temperature Variation at MSL | New on August 1, 2016 |
NASA / JPL-Caltech / Texas A&M
BREAKTHROUGH PROPULSION PHYSICS
Those with an interest in breakthrough propulsion physics should see my notes on the textbook, Frontiers in Propulsion Science (Edited by Marc G. Millis and Eric M. Davis; published by the American Institute of Aeronautics and Astronautics, Inc.). The book, hereafter referred to only as The Textbook, provides information for engineering physics as it relates to spaceship propulsion. It was last updated in 2012. Originally I posted questions (highlighted in red) to pursue at Embry-Riddle Aeronautical University where I earned a B.S. in space physics. However, it only took me 5 semesters to earn my B.S., and much of that time was spent researching the density of the Martian atmosphere. This means that some of the questions remain to be addressed even though I now have my PhD in physics with a specialization in Computational Condensed Matter Theory.
My notes are broken up into sections that match the chapters of The Textbook, with links to the chapter notes in Table 2 below. Comments, corrections, updates to my notes and questions by the AIAA textbook authors or other knowledgeable authorities are most welcome and will be published in the appropriate sections unless they are of a private or potentially classified nature.