Dr. Flores would like an update on your research about what happened to the lake on Titan. Did the lake on Titan evaporate or freeze? After you clearly state your claim, explain how the
evidence connects to the claim to support your argument. Remember to explain what happened
at both the macro and molecular scale.

The lake disappeared during Titan's summer, when the amount of energy being transferred into the lake was higher than at other times, so the lake must have evaporated, not frozen. ... Students figure out: It had been summer since 2002, but the lake didn't evaporate until 2007.

Explanation:

Titan is the only moon in our solar system with a dense atmosphere, which supports an Earth-like cycle of ethane and methane clouds, rain, and liquid that flows into lakes and seas. Examining data from NASA’s Cassini mission, a team led by Shannon MacKenzie of the Johns Hopkins Applied Physics Laboratory in Laurel, Maryland, observed three instances where what appeared to be shallow lakes disappeared between winter and summer — a span of about seven years — in the moon’s northern regions.

“It’s the first time we’ve actually seen a lake on Titan’s surface disappear completely,” said MacKenzie, whose results appear today in Nature Astronomy. “This tells us that if evaporation is happening as slowly as models predict, then the surface must also be porous enough in these areas for liquid to drain into it for the lakes to disappear.”

Understanding the timescales for Titan’s lakes is important for modeling local weather, climate and sediment processing. Titan is the only planetary body in our solar system other than Earth known to have stable liquid on its surface. “These observations give us new insight into the behavior of liquids on Titan’s surface, and how long it takes some of these processes to occur,” MacKenzie said.

MacKenzie added that these processes likely occur at a similar rate across that region on Titan, although it would be harder to observe in the deeper northern lakes. Another Nature Astronomy paper published today, led by Marco Mastrogiuseppe of Caltech in Pasadena, California, reveals that most of the small, liquid lakes in Titan’s northern hemisphere are surprisingly deep, perched atop hills and filled mainly with methane — the first confirmation of just how deep some of the moon’s lakes are (more than 300 feet, or 100 meters) and their composition.

The abundant complex organic material accessible on and just below Titan’s surface makes it an ideal destination for studying the conditions necessary for the habitability of an extraterrestrial environment and the kinds of chemical interactions that occurred before life developed on Earth. A goal of the proposed Dragonfly mission — a rotorcraft-lander concept vying to become NASA’s next New Frontiers mission — would be to sample areas rich with the materials left by liquids that evaporated or seeped into the surface.

Cassini arrived in the Saturn system in 2004 and ended its mission in 2017 by deliberately diving into Saturn’s atmosphere. The spacecraft mapped more than 620,000 square miles (1.6 million square kilometers) of liquid lakes and seas on Titan’s surface. It did the work with the radar instrument, which sent out radio waves and collected a return signal (or echo) that gave information about the terrain and the liquid bodies’ depth and composition, and with two imaging systems that can penetrate the moon’s thick atmospheric haze.

The Cassini-Huygens mission is a cooperative project of NASA, ESA (European Space Agency) and the Italian Space Agency. NASA’s Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, manages the mission for NASA’s Science Mission Directorate. JPL designed, developed and assembled the Cassini orbiter. The radar instrument was built by JPL and the Italian Space Agency, working with team members from the United States and several European countries.

i hope this helps i think

answer: - few nutrients

high pressure

low temperatures

explanation: 1. few nutrients:   open-ocean zone is located way far from the land, which is the main source of the essential nutrients.2. high pressure: pressure increases by 1 atmosphere for every 10 meters increase in depth.3. ample sunlight: a large fraction of the sunlight is reflected back to the atmosphere from the sea surface. 4. varying salinity: below the thermocline, the water is isolated from the atmosphere so the salinity remains stable over the year.5. low temperatures:   the temperature of open-ocean zone ranges from a low of -2°c to an average of 17°c

maritime tropical may be your answer.