Sky Object of the Month – November 2014

NGC 40 – Planetary Nebula in Cepheus
by Glenn Chaple

Our November deep-sky target, NGC 40, could be featured any month of the year. Just 17.5 degrees from the North Celestial Pole, it’s circumpolar from mid-northern latitudes. But it’s during mid autumn that NGC 40’s parent constellation Cepheus rides highest above the northern horizo after sunset.

NGC 40 was discovered by Sir William Herschel on November 25, 1788, and bears the Herschel Catalog designation H IV-58 (his 58th Class IV [Planetary Nebulae] entry). A more recent designation, C2, reflects its inclusion in Sir Patrick Caldwell-Moore’s 1995 Caldwell Catalog – his compilation of the finest 109 non-Messier deep-sky objects. NGC 40 is also nick-named the Bow-Tie Nebula, a moniker it shares with the planetary nebula NGC 2440 in Puppis and the Hubble-imaged protoplanetary nebula PGC 3074547 in Centaurus.

Finding NGC 40 is problematic, as it lies in a star-poor region of Cepheus. The accompanying Telrad chart shows it location about one-third of the way from gamma (() Cephei (labeled Errai) to kappa (() Cassiopeiae. Center your finderscope on the area and begin a low-power search (about 50X should suffice) until you come to what looks like an out-of-focus 12th magnitude star midway between and slightly west of a pair of 9th magnitude stars. NGC 40 can be glimpsed with a 4-inch scope under dark skies, but you’ll need twice that aperture to capture significant detail. Magnifications of 150X and up will reveal a slightly oval 35 X 38 arc second haze surrounding a star of 11.6 magnitude.

If you gaze at NGC 40’s central star, the surrounding nebulosity seems to disappear. Look to the side, and the nebulosity pops into view. The effect mirrors that of NGC 6826 (the “Blinking Planetary” in Cygnus. At a distance of 3500 light years, NGC 40 is about one light year in diameter.

Cosmic Concert Saturday October 11, 7:00

The Gloucester Area Astronomy Club (GAAC) proudly presents a public concert by composer and pianist Bruce Lazarus featuring his major astronomy-themed solo piano work, Musical Explorations of the Messier Catalogue of Star Clusters and Nebulae, Saturday October 11, 2014, 7:00pm, at St Paul Lutheran Church in Lanesville, Massachusetts. Admission is $5.

Musical Explorations of the Messier Catalogue is a series of fourteen pieces inspired by the compilation of astronomical objects of French astronomer Charles Messier (1730-1817). Comet hunter Messier identified, with his small telescope, 110 celestial objects that resembled but were not comets, an extensive numerical "catalogue" of stunning beauty widely used by astronomers of the present day. Composer Lazarus writes of his 45-minute collection, composed between 2004 and 2011:

"Recent Hubble telescope photos of Charles Messier’s list of fuzzy objects in the clear night sky (now known as nebulae, star clusters, galaxies, and immense patches of interstellar gas) reveal vistas of extraordinary beauty and also great variation in energy patterning – spiraling, floating, exploding, diffusing – which suggest musical variations in rhythm, texture, formal design, and melodic elements. I decided to compose a series of musical descriptions of the fourteen most iconic images of these objects: starting with the familiar Andromeda Galaxy (Messier 31), and later moving on to the Orion Nebula (M42), The Pleiades (M45), the most impressive of the globular clusters (M13), the Eagle Nebula with its majestic ‘pillars of star creation,’ and double stars, star clusters, novas and supernovas.

"Following the six-year process of composing my major opus, I switched roles to that of concert pianist recording a CD of the entire cycle, and performing these difficult but very personal scores in public. I am most grateful to GAAC for the opportunity to perform my Messier pieces in Lanesville.”

For directions and a map, click here:

GAAC’s October 11 live Messier performance will be accompanied by projected images of the individual objects. For more information on the Messier pieces, read Bruce Lazarus’ article on the Messier pieces in GAAC’s affiliated eJournal, The Galactic Inquirer.

NASA Spaceplace Partners' Article, September 2014

Twinkle, twinkle, variable star

By Dr. Ethan Siegel

As bright and steady as they appear, the stars in our sky won't shine forever. The steady brilliance of these sources of light is powered by a tumultuous interior, where nuclear processes fuse light elements and isotopes into heavier ones. Because the heavier nuclei up to iron (Fe), have a greater binding energies-per-nucleon, each reaction results in a slight reduction of the star's mass, converting it into energy via Einstein's famous equation relating changes in mass and energy output, E = mc2. Over timescales of tens of thousands of years, that energy migrates to the star's photosphere, where it's emitted out into the universe as starlight.

There's only a finite amount of fuel in there, and when stars run out, the interior contracts and heats up, often enabling heavier elements to burn at even higher temperatures, and causing sun-like stars to grow into red giants. Even though the cores of both hydrogen-burning and helium-burning stars have consistent, steady energy outputs, our sun's overall brightness varies by just ~0.1%, while red giants can have their brightness’s vary by factors of thousands or more over the course of a single year! In fact, the first periodic or pulsating variable star ever discovered—Mira (omicron Ceti)—behaves exactly in this way.

There are many types of variable stars, including Cepheids, RR Lyrae, cataclysmic variables and more, but it's the Mira-type variables that give us a glimpse into our Sun's likely future. In general, the cores of stars burn through their fuel in a very consistent fashion, but in the case of pulsating variable stars the outer layers of stellar atmospheres vary. Initially heating up and expanding, they overshoot equilibrium, reach a maximum size, cool, then often forming neutral molecules that behave as light-blocking dust, with the dust then falling back to the star, ionizing and starting the whole process over again. This temporarily neutral dust absorbs the visible light from the star and re-emits it, but as infrared radiation, which is invisible to our eyes. In the case of Mira (and many red giants), it's Titanium Monoxide (TiO) that causes it to dim so severely, from a maximum magnitude of +2 or +3 (clearly visible to the naked eye) to a minimum of +9 or +10, requiring a telescope (and an experienced observer) to find!

Visible in the constellation of Cetus during the fall-and-winter from the Northern Hemisphere, Mira is presently at magnitude +7 and headed towards its minimum, but will reach its maximum brightness again in May of next year and every 332 days thereafter. Shockingly, Mira contains a huge, 13 light-year-long tail -- visible only in the UV -- that it leaves as it rockets through the interstellar medium at 130 km/sec! Look for it in your skies all winter long, and contribute your results to the AAVSO (American Association of Variable Star Observers) International Database to help study its long-term behavior!

Check out some cool images and simulated animations of Mira here:

Kids can learn all about Mira at NASA’s Space Place:

Images credit: NASA's Galaxy Evolution Explorer (GALEX) spacecraft, of Mira and its tail in UV light (top); Margarita Karovska (Harvard-Smithsonian CfA) / NASA's Hubble Space Telescope image of Mira, with the distortions revealing the presence of a binary companion (lower left); public domain image of Orion, the Pleiades and Mira (near maximum brightness) by Brocken Inaglory of Wikimedia Commons under CC-BY-SA-3.0 (lower right).

September 12 GAAC Meeting Program Note

At our Sept 12 meeting we have a distinguished guest with a great program on how giant, monster galaxies came to be, back at the beginning of everything. This is an important question, one at the forefront of current Hubble discoveries (see image, left).

New ideas on the emergence of these galactic monsters have astronomers rethinking what the very young Universe looked like.

On September 12 Professor Danilo Marchesini of Tufts University will take us back to these primordial times -- and introduce us to the beasts that lit the night skies back then.

Mark your calendars, folks, this will be  a terrific night with an absolutely outstanding presentation by an expert on the subject.

We meet on the second Friday of every month except August, at 8:00 in the Lanesville Community Center. See our Contact page for directions.

And don't forget: we'll see you at the 9/5 HPSP star party!

Sky Object of the Month – September 2014

Messier 22  – Globular Cluster in Sagittarius
by Glenn Chaple

On early evenings in September, the constellation Sagittarius arches above the southern horizon, its rich deep-sky treasures accessible to those of us who inhabit mid-northern latitudes. One of the more spectacular of these cosmic splendors is the globular cluster M22 Its discovery is attributed to the German astronomer Abraham Ihle, who came across it on August 26, 1665 while observing Saturn.

Among globular clusters, M22 is exceeded in brightness and apparent size only by omega Centauri and 47 Tucanae. Much of its grandeur results from its nearness to the earth. At a distance of 10,500 light years, it’s over two times closer than the much-heralded M13. In reality, M13 is half again as large and contains several hundred thousand stars, compared to M22’s estimated 70.000.

I’ve always been a proponent of small telescopes for backyard astronomy, but had to admit that large aperture scopes are the way to go should you want to resolve the stars in a globular cluster. M22 is an exception. I’ve resolved it quite nicely with a 4-inch f/4 RFT (an Edmund Astroscan) and a magnifying power of just 74X.

Naturally, to view M22 in all its glory you’ll want to use a large instrument and 2 or 3 times that magnification.M22 is relatively easy to locate, if you use the “Teapot” of Sagittarius as a guide. In binoculars and finderscopes, it appears as a 5th magnitude smudge just 2 ½ degrees northeast of Kaus Borealis (Lambda [] Sagittarii) - a 3rd magnitude star that forms the top of the Teapot’s lid. Next time you’re visiting M13, drop southward and give M22 a look-see. Which do you prefer?

Chart credit: photo by Mario Motta, MD

NASA Spaceplace Partners' Article, August 2014

Droughts, Floods and the Earth's Gravity, by the GRACE of NASA
By Dr. Ethan Siegel

When you think about gravitation here on Earth, you very likely think about how constant it is, at 9.8 m/s2 (32 ft/s2). Only, that's not quite right. Depending on how thick the Earth's crust is, whether you're slightly closer to or farther from the Earth's center, or what the density of the material beneath you is, you'll experience slight variations in Earth's gravity as large as 0.2%, something you'd need to account for if you were a pendulum-clock-maker.

But surprisingly, the amount of water content stored on land in the Earth actually changes the gravity field of where you are by a significant, measurable amount. Over land, water is stored in lakes, rivers, aquifers, soil moisture, snow and glaciers. Even a change of just a few centimeters in the water table of an area can be clearly discerned by our best space-borne mission: NASA's twin Gravity Recovery and Climate Experiment (GRACE) satellites.

Since its 2002 launch, GRACE has seen the water-table-equivalent of the United States (and the rest of the world) change significantly over that time. Groundwater supplies are vital for agriculture and provide half of the world's drinking water. Yet GRACE has seen California's central valley and the southern high plains rapidly deplete their groundwater reserves, endangering a significant portion of the nation's food supply. Meanwhile, the upper Missouri River Basin—recently home to severe flooding—continues to see its water table rise.

NASA's GRACE satellites are the only pieces of equipment currently capable of making these global, precision measurements, providing our best knowledge for mitigating these terrestrial changes. Thanks to GRACE, we've been able to quantify the water loss of the Colorado River Basin (65 cubic kilometers), add months to the lead-time water managers have for flood prediction, and better predict the impacts of droughts worldwide. As NASA scientist Matthew Rodell says, "[W]ithout GRACE we would have no routine, global measurements of changes in groundwater availability. Other satellites can’t do it, and ground-based monitoring is inadequate." Even though the GRACE satellites are nearing the end of their lives, the GRACE Follow-On satellites will be launched in 2017, providing us with this valuable data far into the future. Although the climate is surely changing, it's water availability, not sea level rise, that's the largest near-term danger, and the most important aspect we can work to understand!

Learn more about NASA’s GRACE mission here:

Kids can learn al about launching objects into Earth’s orbit by shooting a (digital) cannonball on NASA’s Space Place website. Check it out at:

Image credit: NASA Earth Observatory image by Jesse Allen, using GRACE data provide courtesy of Jay Famigleitti, University of California Irvine and Matthew Rodell, NASA Goddard Space Flight Center. Caption by Holli Riebeek.

NASA Spaceplace Partners' Article, July 2014

The Invisible Shield of our Sun

By Dr. Ethan Siegel

Whether you look at the planets within our solar system, the stars within our galaxy or the galaxies spread throughout the universe, it's striking how empty outer space truly is. Even though the largest concentrations of mass are separated by huge distances, interstellar space isn't empty: it's filled with dilute amounts of gas, dust, radiation and ionized plasma. Although we've long been able to detect these components remotely, it's only since 2012 that a manmade spacecraft -- Voyager 1 -- successfully entered and gave our first direct measurements of the interstellar medium (ISM).

What we found was an amazing confirmation of the idea that our Sun creates a humongous "shield" around our solar system, the heliosphere, where the outward flux of the solar wind crashes against the ISM. Over 100 AU in radius, the heliosphere prevents the ionized plasma from the ISM from nearing the planets, asteroids and Kuiper belt objects contained within it. How? In addition to various wavelengths of light, the Sun is also a tremendous source of fast-moving, charged particles (mostly protons) that move between 300 and 800 km/s, or nearly 0.3% the speed of light. To achieve these speeds, these particles originate from the Sun's superheated corona, with temperatures in excess of 1,000,000 Kelvin!

When Voyager 1 finally left the heliosphere, it found a 40-fold increase in the density of ionized plasma particles. In addition, traveling beyond the heliopause showed a tremendous rise in the flux of intermediate-to-high energy cosmic ray protons, proving that our Sun shields our solar system quite effectively. Finally, it showed that the outer edges of the heliosheath consist of two zones, where the solar wind slows and then stagnates, and disappears altogether when you pass beyond the heliopause.

Unprotected passage through interstellar space would be life-threatening, as young stars, nebulae, and other intense energy sources pass perilously close to our solar system on ten-to-hundred-million-year timescales. Yet those objects pose no major danger to terrestrial life, as our Sun's invisible shield protects us from all but the rarer, highest energy cosmic particles. Even if we pass through a region like the Orion Nebula, our heliosphere keeps the vast majority of those dangerous ionized particles from impacting us, shielding even the solar system's outer worlds quite effectively. NASA spacecraft like the Voyagers, IBEX and SOHO continue to teach us more about our great cosmic shield and the ISM's irregularities. We're not helpless as we hurtle through it; the heliosphere gives us all the protection we need!

Want to learn more about Voyager 1’s trip into interstellar space? Check this out:

Kids can test their knowledge about the Sun at NASA’s Space place:

Image credit: Hubble Heritage Team (AURA / STScI), C. R. O'Dell (Vanderbilt), and NASA, of the star LL Orionis and its heliosphere interacting with interstellar gas and plasma near the edge of the Orion Nebula (M42). Unlike our star, LL Orionis displays a bow shock, something our Sun will regain when the ISM next collides with us at a sufficiently large relative velocity.

GAAC July Meeting, "Astrophotography, From Beginner to Expert"

The 8:00 pm Friday July 11 meeting of the Gloucester Area Astronomy Club is a free astrophoto festival, filled with outstanding photos of planets, and immense, distant, colorful galaxies, nebulae, and star clusters, shown on GAAC's 100 inch screen! The meeting will feature in-person presentations by four outstanding photographers, showing off their best work, and an introduction by our own Steve K, who will demonstrate how simple astrophotography can be for beginners.

Photographers Mario Motta, Phil Orbanes, John Hobbs and Barry Yomtov will each present their ten favorite pictures, and will talk briefly about what the objects are, how far away they are, how big, and a little about why and how each person got that shot.

This will be a spectacular, colorful night, with great presenters, and we'll have a wonderful time getting a rare, entertaining and accessible look into the world of astrophotography. Many of the photographs can be previewed in the Gallery section of this website.

The club meets on the second Friday of every month at the Lanesville Community Center, 8 Vulcan Street Lanesville, from 8:00 to 9:30 pm. Parking is free. The public is warmly welcomed and there is no cost. More information is available through the website, or on Facebook at or in the club twitter feed, @gaactweet.