Astronomy Habitable Zone
Astronomy Habitable Zone
Astronomy Habitable Zone , The presence of liquid water is considered to be a prerequisite for life as we know it, which makes looking for water a practical way to begin our search for life beyond Earth. For water to exist on the surface of a planet, the planet must have the right temperature on its surface. The main driving force behind the surface temperature of any planet is the light it receives from its parent star. Around every star there is a region where the planet will receive just the right amount of light to give it temperatures that are conducive to liquid water – this region is call the star’s Habitable Zone. The orbit of the Earth currently falls within the Habitable Zone of our Sun.
2 The Habitability of the Earth
To begin, load up the Habitable Zone simulator written by the University of Nebraska by entering the following URL in the address bar of your web browsers:
The flash simulator will show you a visual diagram of the solar system in the top panel, a set of simulation settings in the middle panel, and a timeline of the habitability of the Earth in the bottom panel. To run the simulation, click the run in the bottom panel. This button immediately becomes a pause button which will allow you to pause the simulation at any time. To restart the simulation, press the restart button at the very top of the simulation.
The blue region marked on the diagram is the Habitable Zone around our Sun. Notice how there is both an inner edge and an outer edge – the planets interior to the habitable zone are too hot to support liquid water, while the planets exterior to it are too cold.
1) The simulation is currently set to zero-age – this is the Solar System as it was when it first formed, 5 billion years ago. Which planets were in the Habitable Zone at this time?
2) Press the start button and watch the Habitable Zone change with time. Pause the simulation when it reaches an age of 5 billion years (you can keep track of the time by looking at the timeline marker in the bottom panel). This is the Solar System as it is today – which planets are in the Habitable Zone now?
3) Allow the simulation to run until the Earth is no longer in the Habitable Zone. At what age does this happen? How long from now until this happens? You can use the timeline bar in the bottom panel to determine your answers. .
4) After the Earth is no longer within the Habitable Zone, what do you think the condi- tions on Earth will be like?
5) Resume the simulation and let it run until the end. Which planets other than the Earth fell within the Habitable Zone at any point during the Sun’s life?
6) If you had to choose planets of our Solar System for future colonization based on their future habitability, which would you choose, and why?
3 The Habitability Different Kinds of Stars
Now that you’ve simulated the Habitable Zone around our Sun, we’ll run the same simulation for other stars. Astronomers classify stars with letters, O, B, A, F, G, K, and M. The O stars are the hottest and brightest, while the M stars are the dimmest and coolest. Every kind of star has a Habitable Zone, but the brighter the star the farther out the Habitable Zone. Imagine putting and extra log on a campfire – the campers all have back off a few feet to maintain the same comfortable temperature.
But in order for complex life to have a chance to develop, a planet must remain habitable for an extended period of time. How long? We only have Earth to use as an example, so we really don’t know. For the purpose of this exercise, we’ll assume that Earth is “typical” and that planets around other stars mostly follow the timeline of events on Earth shown below:
2 Billions of Years Ago Development Toward Complex Life 4.5 Earth forms 4.3-4.4 Earth cools, oceans form 3.8 first bacterial fossils 2.4 rise of oxygen in atmosphere 2.0 first complex cells 0.55 first complex animals (fossils in Clapp)
The next table shows several different kinds of stars. Notice how they each have a different mass – the mass of a star determines what kind of a star it is. Reset the Habitable Zone simulator with the reset button at top, and then adjust the star mass with the initial star mass slider bar in the middle panel. Notice how the Habitable Zone immediately changes size. Notice also that you can adjust the orbit of “Earth” by adjusting the initial planet distance slider bar in the middle panel. The units of distance from the star are AU – astronomical units, the distance of the Earth from the Sun. The Earth is one AU from the Sun.
For each of the star types in the table below, find the planet orbit that remains habitable the longest. To do this you’ll need to run the simulation many times for each star type, each time adjusting the initial planet distance until you find a distance that keeps the planet habitable the longest. Record in the table 1) the size of this orbit, in AU, 2) how long this orbit remains habitable, 3) the most advanced type of life that can develop during this time frame, assuming the Earth’s timeline for life is typical.
Type Star Mass Longest Habitable Orbit Habitable Lifetime Most Advanced Life [Solar Masses] [Astronomical Units] [Billions of Years]
O 15. B 5.0 A 2.0 F 1.3 G (Sun) 1.0 K 0.7 M 0.4
4 Tidal Locking
Unfortunately, for low-mass M type stars the habitable zone is quite close to the star – so close that planets in this zone are likely to be tidally locked. This means that the same side of the planet will always face the star, just as the same side of the Earth’s moon always faces the Earth. The simulator indicates that a planet is tidally locked when it is split between one brown and the other side being light gray. In this section we’ll experiment with planets around M type stars. Adjust the stars “initial stellar mass” to 0.3 (30% of the Sun’s mass), and adjust the “initial planet distance” until the planet is in the star’s Habitable Zone. The planet should switch to the tidally locked icon, even if the planet is in the Habitable Zone.
1) What impact do you think tidal locking would have on the prospect of life on this planet?
2) Try adjusting the star’s mass. What is the lowest mass star that would allow a non- tidally locked planet in the Habitable Zone at the beginning of the star’s life?
3) What is the lowest mass star that would allow a non-tidally locked planet in the Hab- itable Zone at any point during the star’s life?
5 Tying it All Together
1) Given what you’ve learned so far, what type of star is the best place to look for life?
2) The Sun is a G-type star. What do you think the development of life on planets orbiting hotter types of stars would be like? What about cooler types of stars? Do you think that life in such conditions is even possible? Justify your answer.
3) If you were the director of a NASA program to search for life beyond Earth, toward which type of star would you direct your attention? Why? Justify your answer using the evidence above, and also any other lines of reasoning you like. Help Me Write My Essay