Abstract

First global map of Venus nightside surface temperature using Akatsuki infrared measurements reveals hot Venus surface with an average surface temperature of about 698 K. Surface temperatures do not show any significant variation with changing latitudes because only a small amount (~2.5%) of solar energy reaches the surface. Surface temperatures are relatively colder at higher altitude regions as compared to lower altitude regions. However, the major temperature variation on Venus surface is governed by various lithospheric heat transport mechanisms. On a global scale, surface temperatures show a spatial variation of about 230 K.

Highlights

  • In our solar system, Venus is the second planet and orbiting at a distance of about 0.72 AU from Sun

  • I focus my work on retrieving nightside surface temperatures of Venus because 0.90 μm dayside channel detects solar radiation due to cloud scattering[5,6]

  • Since most of Venus surface is covered by regional flat plains, the entire surface temperature range occurs within 2 km of zero altitude surface (Fig. 4)

Read more

Summary

OPEN Venus nightside surface temperature

First global map of Venus nightside surface temperature using Akatsuki infrared measurements reveals hot Venus surface with an average surface temperature of about 698 K. Surface temperatures do not show any significant variation with changing latitudes because only a small amount (~2.5%) of solar energy reaches the surface. Venus is similar to Earth in terms of size (0.95 of Earth’s radius), mass (0.814 of Earth’s), bulk density (0.95 of Earth’s), and gravity (0.907 of Earth’s). Due to these similarities Venus is considered as ‘twin-planet’ of Earth. I focus this work in retrieving Venus surface temperature to improve our understanding, and to constrain its variability. I focus my work on retrieving nightside surface temperatures of Venus because 0.90 μm dayside channel detects solar radiation due to cloud scattering[5,6]. More than 95% of the radiation measured in IR1 window comes from Venus surface[7], and the interference caused by cloud inhomogeneity appears to be insignificant[6]

Nightside Surface Temperature Of Venus
Conclusions
Methods
Findings
Additional Information

Talk to us

Join us for a 30 min session where you can share your feedback and ask us any queries you have

Schedule a call

Disclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.