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Related Experiment Video

Updated: Dec 29, 2025

Exploring the Effects of Atmospheric Forcings on Evaporation: Experimental Integration of the Atmospheric Boundary Layer and Shallow Subsurface

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Relative Humidity on Mars: New Results From the Phoenix TECP Sensor.

E Fischer¹, G M Martínez^1,2, N O Rennó¹

¹Department of Climate and Space Sciences and Engineering University of Michigan Ann Arbor MI USA.

Journal of Geophysical Research. Planets

|February 7, 2020

Summary

Recalibrated Phoenix lander humidity sensors show higher daytime water vapor pressure on Mars. This suggests stronger atmosphere-regolith interaction in the Martian arctic, impacting potential brine formation.

Keywords:

Mars Phoenix TECP relative humidity water cycle water vapor

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Published on: March 25, 2019

Area of Science:

Planetary Science
Atmospheric Science on Mars
Astrobiology

Background:

In situ relative humidity (RH) measurements on Mars are limited, primarily from Phoenix (PHX) and Mars Science Laboratory (MSL) missions.
Previous calibrations of the PHX Thermal and Electrical Conductivity Probe (TECP) RH sensor did not fully cover warm, dry daytime Martian conditions.
Understanding Mars' near-surface humidity is crucial for assessing habitability and geological processes like brine formation.

Purpose of the Study:

To recalibrate the PHX TECP RH sensor, focusing on environmental conditions not covered in prior calibrations.
To improve the accuracy of RH measurements for the PHX mission, particularly during daytime.
To investigate the diurnal and latitudinal variations in Martian water vapor pressure and their implications.

Main Methods:

Recalibration of a TECP engineering model using environmental conditions from the PHX landing site in the Michigan Mars Environmental Chamber.
Experiments focused on simulating the warmest and driest Martian daytime conditions.
Comparison of recalibrated data with previous calibrations and independent measurements from PHX instruments and orbital data.

Main Results:

Recalibration yielded higher daytime water vapor pressure values (~0.005–1.4 Pa) compared to previous estimates (~0.004–0.4 Pa).
Nighttime RH measurements showed excellent agreement with the 2016 recalibration.
Higher daytime values align better with independent surface and orbital measurements, suggesting enhanced atmosphere-regolith water vapor exchange at PHX.

Conclusions:

The recalibrated sensor data indicate larger day-to-night water vapor pressure ratios at the PHX site compared to MSL.
These findings suggest a stronger atmosphere-regolith interchange in the Martian arctic than at lower latitudes.
Brine formation via deliquescence at the PHX site is likely a temporary, nocturnal phenomenon.