(PhysOrg.com) -- The sinking of the ocean liner Titanic 100 years ago is perhaps the most famous--and most studied--disaster of the 20th century. Countless books and movies have examined in great detail the actions, choices and mistakes that led to the Titanic colliding with an iceberg the night of April 14, 1912, and sinking within hours, with approximately 1,500 people losing their lives in the icy waters of the North Atlantic. googletag.cmd.push(function() googletag.display('div-gpt-ad-1449240174198-2'); ); One question, however, has often been overlooked: Where did the killer iceberg come from, and could the moon have helped set the stage for disaster?Now, a team of astronomers from Texas State University-San Marcos has applied its unique brand of celestial sleuthing to the disaster to examine how a rare lunar event stacked the deck against the Titanic. Their results shed new light on the hazardous sea ice conditions the ship boldly steamed into that fateful night.Texas State physics faculty members Donald Olson and Russell Doescher, along with Roger Sinnott, senior contributing editor at Sky & Telescope magazine, publish their findings in the April 2012 edition of Sky & Telescope, on newsstands now.“Of course, the ultimate cause of the accident was that the ship struck an iceberg. The Titanic failed to slow down, even after having received several wireless messages warning of ice ahead,” Olson said. “They went full speed into a region with icebergs—that’s really what sank the ship, but the lunar connection may explain how an unusually large number of icebergs got into the path of the Titanic.” This map shows the known route of the Titanic and a possible path for the iceberg. We will never know the iceberg's actual trajectory, but modern knowledge of currents and drift patterns make this a highly plausible scenario. Had it not been for the enhanced tidal effects a few months earlier, the iceberg might have run aground on the Labrador or Newfoundland coast, and remained permanently stuck until it melted. A tide for the agesInspired by the visionary work of the late oceanographer Fergus J. Wood of San Diego who suggested that an unusually close approach by the moon on Jan. 4, 1912, may have caused abnormally high tides, the Texas State research team investigated how pronounced this effect may have been.What they found was that a once-in-many-lifetimes event occurred on that Jan. 4. The moon and sun had lined up in such a way their gravitational pulls enhanced each other, an effect well-known as a “spring tide.” The moon’s perigee—closest approach to Earth—proved to be its closest in 1,400 years, and came within six minutes of a full moon. On top of that, the Earth’s perihelion—closest approach to the sun—happened the day before. In astronomical terms, the odds of all these variables lining up in just the way they did were, well, astronomical.“It was the closest approach of the moon to the Earth in more than 1,400 years, and this configuration maximized the moon’s tide-raising forces on Earth’s oceans. That’s remarkable,” Olson said. “The full moon could be any time of the month. The perigee could be any time of the month. Think of how many minutes there are in a month.”Initially, the researchers looked to see if the enhanced tides caused increased glacial calving in Greenland, where most icebergs in that part of the Atlantic originated. They quickly realized that to reach the shipping lanes by April when the Titanic sank, any icebergs breaking off the Greenland glaciers in Jan. 1912 would have to move unusually fast and against prevailing currents. But the ice field in the area the Titanic sank was so thick with icebergs responding rescue ships were forced to slow down. Icebergs were so numerous, in fact, that the shipping lanes were moved many miles to the south for the duration of the 1912 season. Where did so many icebergs come from? (adsbygoogle = window.adsbygoogle []).push(); Icebergs run agroundAccording to the Texas State group, the answer lies in grounded and stranded icebergs. As Greenland icebergs travel southward, many become stuck in the shallow waters off the coasts of Labrador and Newfoundland. Normally, icebergs remain in place and cannot resume moving southward until they’ve melted enough to refloat or a high enough tide frees them. A single iceberg can become stuck multiple times on its journey southward, a process that can take several years. But the unusually high tide in Jan. 1912 would have been enough to dislodge many of those icebergs and move them back into the southbound ocean currents, where they would have just enough time to reach the shipping lanes for that fateful encounter with the Titanic.“As icebergs travel south, they often drift into shallow water and pause along the coasts of Labrador and Newfoundland. But an extremely high spring tide could refloat them, and the ebb tide would carry them back out into the Labrador Current where the icebergs would resume drifting southward,” Olson said. “That could explain the abundant icebergs in the spring of 1912. We don’t claim to know exactly where the Titanic iceberg was in January 1912—nobody can know that--but this is a plausible scenario intended to be scientifically reasonable.” Provided byTexas State University
Unlike all the other stars in this picture, which are close by in the foreground of our own Milky Way Galaxy, that one star indicated is 38 million light years away. It lies in another galaxy altogether, in the outer spiral arm of the galaxy M95. Discovered on March 16, Supernova SN 2012aw is now shining with the light of a hundred million suns as it blasts most of its starstuff into space.
Sky And Telescope - April 2012
The L/M-band (3-5 μm) InfraRed Camera (LMIRcam) sits at the combined focal plane of the Large Binocular Telescope Interferometer (LBTI), ultimately imaging the coherently combined focus of the LBT's two 8.4-meter mirrors. LMIRcam achieved first light at the LBT in May 2011 using a single AO-enabled 8.4-meter aperture. With the delivery of LBT's final adaptive secondary mirror in Fall of 2011, dual-aperture AO-corrected interferometric fringes were realized in April 2012. We report on the performance of these configurations and characterize the noise performance of LMIRcam's HAWAII-2RG 5.3-μm cutoff array paired with Cornell FORCAST readout electronics. In addition, we describe recent science highlights and discuss future improvements to the LMIRcam hardware.
N2 - The L/M-band (3-5 μm) InfraRed Camera (LMIRcam) sits at the combined focal plane of the Large Binocular Telescope Interferometer (LBTI), ultimately imaging the coherently combined focus of the LBT's two 8.4-meter mirrors. LMIRcam achieved first light at the LBT in May 2011 using a single AO-enabled 8.4-meter aperture. With the delivery of LBT's final adaptive secondary mirror in Fall of 2011, dual-aperture AO-corrected interferometric fringes were realized in April 2012. We report on the performance of these configurations and characterize the noise performance of LMIRcam's HAWAII-2RG 5.3-μm cutoff array paired with Cornell FORCAST readout electronics. In addition, we describe recent science highlights and discuss future improvements to the LMIRcam hardware.
AB - The L/M-band (3-5 μm) InfraRed Camera (LMIRcam) sits at the combined focal plane of the Large Binocular Telescope Interferometer (LBTI), ultimately imaging the coherently combined focus of the LBT's two 8.4-meter mirrors. LMIRcam achieved first light at the LBT in May 2011 using a single AO-enabled 8.4-meter aperture. With the delivery of LBT's final adaptive secondary mirror in Fall of 2011, dual-aperture AO-corrected interferometric fringes were realized in April 2012. We report on the performance of these configurations and characterize the noise performance of LMIRcam's HAWAII-2RG 5.3-μm cutoff array paired with Cornell FORCAST readout electronics. In addition, we describe recent science highlights and discuss future improvements to the LMIRcam hardware.
CCD-wise, I observe with telescope time bought on commercial remote telescopes operated by iTelescope and Sierra Stars. For example, I've been observing some of the stars on a programme of 50 underobserved Miras run in collaboration with a number of fellow Swedish variabilists. The list of programme stars was chosen by Hans Bengtsson (BHS) on the criteria that they have no or very few observations in the AID, be fairly bright at maximum, and be distributed throughout the sky, so that some is available for observation at any time. We've had very good help from the AAVSO sequence team in getting sequences for these stars set up!
The 16-inch telescope at the Missouri University of Science and Technology Observatory will be set up to view Venus and Mars, the two brightest planets in the sky, on Friday, April 20. Doors will open at 8 p.m. The sky must be clear for observing and session length will vary. This will be the final viewing of the spring semester.
In 2020 I worked with Radian Telescopes to develop my own signature refractor telescope, the Radian 61 APO. This triplet apochromatic refractor has a wide focal length of 250mm, and an f-ratio of F/4.5.
The type of telescope you choose early on can have a dramatic impact on the complexity of your deep-sky astrophotography setup. In my experience, a compact, wide-field refractor offers an improved user experience over the other telescope types during the acquisition stages of astrophotography.
For example, I began taking my first deep-space images with a reflector telescope. If I could go back and I do it all over again, I would have chosen a compact, wide-field refractor to start astrophotography with.
I often see newcomers to deep-sky astrophotography starting with a telescope that will make an already challenging hobby even more difficult. I went through this experience personally, and this is what happened. 2ff7e9595c
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