ASTR/GEOL-2040: Search for life in the Universe: Lecture 11

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Presentation transcript:

ASTR/GEOL-2040: Search for life in the Universe: Lecture 11 Habitable words Habitable zones temperatures elsewhere ASTR-2040: Lecture 8, Feb 9, 2017

Background reading RGS pp.43 – 50 Longstaff p. 352

Habitable world Dec 16, 1992 Galileo Earth: today very different Liquid water Fluorescense UV  O2 Phytoplankton

Earth’s color Fluorescense in UV  O2 Apollo 16, 50-150 nm Worked with film

Phytoplankton

Phytoplankton reflects green Important in modern times: 50-85% of worlds O2 Fe as nutrient

Diatoms Unicellular 2-200 mm eukarya

Chlorophyll Two types a & b red & blue Complement

Atmosphere not stable O2 continuously regenerated Sea viewing wide field sensor Atmosphere not stable O2 continuously regenerated

Defining habitable planet Special reference to our world Land & oceans O2 continuously regenerated Some O3 protects from UV Liquid water  habitable zone (HZ)

Motivation: TRAPPIST-1 M8 star 7 terrestrial planets m=18.8, 12 pc = 39 ly

L=4pr2F Extremophiles Preparation for midterm exam Midterm exam on Thursday

Trappist-1: an ultra-cold star Extremophiles Preparation for midterm exam Midterm exam on Thursday

TRAPPIST-1 vs Sun Extremophiles Preparation for midterm exam Midterm exam on Thursday

Transits Orbits: 1.5-14 days Host star infrared

What determines Earth’s temperature? ….. ….. ….. ….. …... ……

What determines Earth’s temperature? ….. ….. ….. ….. …... …… If each of you got the same amount of money how much will each of you have?

The Earth loses more energy when the surface is cold the surface is hot neither: it loses a fixed amount

Color of “black” body

The hotter, the more 100 K 1000 K 10,000 K

The hotter, the more 100 K  5.67 1000 K  56,700 10,000 K 

Intermediate numbers 100 K 178 K 316 K 562 K 1000 K 10,000 K

Next time Finish temperature calculation Carbon cycle Plate tectonics pp. 50 - 53

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