William Herschel, A Man for All Seasons

Located about 100 miles west of London, the city of Bath is known for the ancient Roman Baths that attract 1 million visitors each year.  One half mile west from the baths is the Herschel Museum of Astronomy, the 18th century residence of William Herschel.  As an observational astronomer, William Herschel tends to get overlooked by the great theorists such as Issac Newton.  Nonetheless, the work Herschel did in Bath greatly expanded our knowledge of the universe and remains topical in astronomy research.

In contemporary parlance, Herschel was a career changer.  Originally a musician by trade, Herschel took an interest in astronomy in 1773 at the age of 35.  Herschel was a self-made man.  He had no formal training in astronomy and taught himself the art of telescope making.  What had perked Herschel’s interest in astronomy was a book on musical mathematics called Harmonics by Robert Smith.  Herschel enjoyed the book so much he sought out other books by Smith and found one titled Opticks.  This book, along with Astronomy by James Ferguson, formed the basis of Herschel’s training in the field.  Herschel remained a music teacher during the the day and astronomer at night.  In his endeavors he was joined by his sister, Caroline Herschel, who became his lifelong assistant.

Above:  Herschel’s Symphony No. 8 in C minor by London Mozart Players.  Written in 1761, it is one of 24 symphonies composed by William Herschel.

Herschel was unable to buy a telescope suitable for his ambitions.  As a result, along with his sister Caroline, he took to the task of making his own telescopes.  Astronomers today do not need to do this obviously, but this is similar to the manner many astronomers write their own computer codes for their work.  This type of specialized software is not available at a store in your local shopping mall.  Over his lifetime, Herschel would grind and polish hundreds of mirrors, some of which he sold to help fund his work.

Herschel’s primary goal was quite formidable, to conduct an all-sky survey.  Motorized drives to track objects as they moved in the night sky were not available in the 19th century, so Herschel would observe at a fixed angle on the meridian and logged objects as they crossed the field of view.  The next evening, Herschel would lower or raise the telescope to a different angle for complete coverage of the night sky.   This effort resulted in the publication of the Catalogue of Nebulae and Clusters of Stars (CN) in 1786, the forerunner of the New General Catalouge (NGC).  Along the way, Herschel would make quite a few interesting discoveries.

On the night of March 13, 1781, from his residence in Bath, Herschel observed in his 6-inch telescope what he thought was a comet.  Herschel noted:

“On Tuesday, the 13th of March, 1781, between ten and eleven in the evening, while I was examining the small stars in the neighborhood of H Geminorum, I perceived one that appeared visibly larger than the rest: being struck with its uncommon magnitude, I compared it to H Geminorum and the small star in the quartile between Auriga and Gemini, and finding it so much larger than either of them, suspected it to be a comet.”

Measurements of the orbit of this object revealed it to be not a comet, but a planet, the first planet discovered since the ancient astronomers categorized the five naked eye planets of Mercury, Venus, Mars, Jupiter, and Saturn.  Below is an image of how the night sky appeared in Bath as Herschel made his first observation of this planet.

UranusHerschel wanted to call this planet Georgium Sidus (The Georgian Star) to honor King George III.  Others sought a less English-centric name.  Uranus was proposed as in Greek mythology, Uranus is the father of Saturn.  It was not until 1850 that the planet was officially designated as Uranus.  As Uranus is twice the distance (1,783,939,400 miles or 2,870,972,200 km) to the Sun as Saturn, this discovery doubled the size of the known Solar System.  It takes 84 years for Uranus to orbit the Sun.  Thus, Uranus has only made 2.8 revolutions of the Sun since its discovery.  In 1986, Voyager II would become the only spacecraft to date to pay a visit to Uranus.  A view of Uranus from Voyager II is below:

Uranus on January 1986. Image on right is false color to enhance color differentials. The South Pole (red) is darker than equatorial regions. Credit: NASA/JPL.

Uranus’  South Pole was facing Voyager II as it is inclined 98 degrees compared to Earth’s 23.5 degree axial tilt.  If Earth had the same axial tilt as Uranus, the Northern Hemisphere would face the Sun in June while the entire Southern Hemisphere would be in darkness.  The situation would be reversed in December.  When Voyager II flew past Uranus, the Northern Hemisphere was shrouded in darkness.  If NASA’s plans to send an orbiter around Uranus comes to fruition in the 2030’s, the Northern Hemisphere would then be visible.

This discovery was a game changer for Herschel.  King George III, as the Revolutionary War raged in the American colonies, provided Herschel with a salary to pursue astronomy on a full-time basis.  This would launch Herschel on a decade of discovery.

In 1784, Herschel published On the Remarkable Appearances at the Polar Regions on the Planet MarsThis paper presented the results of observations taken of Mars from 1777 to 1783.  A few of Herschel’s drawings of Mars is below:

Credit: Royal Astronomical Society
Credit: Royal Astronomical Society

Among the conclusions Herschel came to from these observations are:

The axial tilt of Mars is 280 42′, reasonably close to the now established value of 25 degrees.

The length of the Martian day as 24 hours, 39 minutes, and 21 seconds.  This measurement was off by only 2 minutes.

The luminous areas at the polar regions were ice caps, which like Earth, would vary in size on a seasonal basis.  Today, we know the northern ice cap has a permanent layer of water ice.  The southern ice cap has a permanent top layer of 8 meters of carbon dioxide ice and a much larger layer of water ice below.  The seasonal variations of the ice caps are due to the freezing and evaporation of carbon dioxide ice.

Herschel concluded his paper by stating, “And the planet has a considerable but moderate atmosphere, so that its inhabitants probably enjoy a situation in many respects similar to our own.” Ok, this one didn’t quite pan out as we know Mars’ mostly carbon dioxide atmosphere is much thinner than Earth’s and life does not exist on the surface.  However, Mars atmosphere in its ancient past must have been warmer and more substantial for water to have been present on the surface, of which the evidence is now pretty conclusive.  The search for life in Mars’ past and microbial life in the Martian sub-surface, which still has water, is a major component in NASA’s Mars Exploration Program.

While several rovers and orbiters have provided thousands of high resolution images of Mars, Earth bound telescopes still acquire key data on Mars past and present:

 

Herschel would also discover two moons of both Saturn and Uranus.

The Uranus moons were discovered on the same day in 1787 and were named Titania and Oberon.  Both moons were imaged by Voyager II on its flyby of Uranus.  Titania featured fault valleys as long as 1,500 km and Oberon has a mountain 4 miles high.

Titania taken by Voyager II 369,000 km (229,000 miles). Credit: NASA/JPL

Two years later, Herschel would discover the Saturn moons Mimas and Enceladus.  Both these moons have been imaged by the Cassini orbiter mission.  Mimas features a large impact crater that has given it the nickname “Death Star”.

Mimas, whose crater gives it a resemblance to the Star Wars Death Star. Credit: NASA/JPL/SSI

The crater has been named in Herschel’s honor.  The crater itself is 140 km (88 miles) wide and the outer walls are 5 km high with a central peak 6 km high.  An impact just a bit larger would have most likely destroyed Mimas.  As interesting as this is, it is Enceladus that has proven to be one of the biggest surprises of the Cassini mission.

Only 500 km wide, Enceladus is very bright as it reflects almost 100% of the sunlight it receives.  Thought to be too small for geologic activity, Enceladus provided an unexpected finding when Cassini imaged geysers spraying ice and water vapor into space.  Further gravity analysis indicates an ocean 10 km deep underneath a ice shell 30-40 km deep.  Recently, it has been determined the geysers are more akin to curtain eruptions seen in volcanic activity in Hawaii and Iceland.  Still, this water is thought to be at least 194 degrees Fahrenheit at the ocean floor, the heat generated by gravitational flexing from Saturn.  Where there is heat and water, there may be life.  Cassini has flown through the geysers but its instrument package was not specifically designed for this task.  As such, Enceladus is a priority for NASA exploration in the next decade.  Unlike the subsurface ocean of Europa, the ocean of Enceladus could be sampled without having to bore down through several kilometers of ice.

Plumes of water ice emanating from the south pole of Enceladus. Credit: NASA/JPL/Space Science Institute.

As impressive as Herschel’s Solar System discoveries were, the task to complete an all-sky survey meant he studied deep space objects moreso than planets and their satellites.  Herschel would discover numerous nebulae and binary stars that prior to his telescope, were not resolvable.  By 1785, with the salary granted by King George III, Herschel had moved from Bath to London and was using a 19-inch aperture telescope to map the Milky Way.  The results were published as On the Construction of the Heavens.  

Credit: Royal Astronomical Society.
Credit: Royal Astronomical Society.

The bright spot in the center is the Sun.  Herschel was operating under the handicap of observing in visible light only, which is extinguished by the interstellar medium.  This gave the illusion the Sun was located in the center of the Milky Way as the interstellar medium dampened optical light in all directions equally.  It is like trying to map trees in a foggy forest.  There may be more trees in one direction than the other, but the fog cuts down on your vision at equal depths in all directions.  In fact, it was not until the 1920’s when Harlow Shapley determined the Sun was located in a spiral arm of the Milky Way  and not in the center was this problem resolved.  For astronomers to obtain a comprehensive view of the universe, the entire electromagnetic spectrum had to be employed.  And it was Herschel who provided the first step in that direction.

In 1800, Herschel was measuring the temperatures of the different colors of sunlight separated by a prism.  As Herschel took temperatures from the violet end of the spectrum to the red he discovered an increase in temperature as the thermometer was moved towards the red.  Finally, the thermometer was placed just beyond the red light, and the temperature increased even more.  It was apparent the Sun was emitting some form of radiation beyond the furthest end of the visible spectrum.  More experiments revealed this invisible radiation had the same properties as visible light, it could be reflected and refracted.  Herschel published this result in the paper titled, Experiments on the Refrangibility of the Invisible Rays of the Sun.  Herschel referred to this radiation as calorific (heat) rays, today we call it infrared light.

Credit: NASA

Optical light is just a small part of the electromagnetic spectrum.  Among the other parts we are unable to detect with our eyes, we can detect radio waves with radio receivers, ultraviolet waves with our skin when we get sunburn, and x-rays with film when we go to the doctor.  Those forms of radiation only differ from light in the size of their respective wavelengths and consequently, their energy.  Infrared is used for remote control and night vision technology. Most of the heat we feel in our day-to-day activities is the result of infrared light and our bodies emit infrared radiation in the form of body heat which is detected in night vision sensors.

Cat in infrared. Eyes appear warmer than body as cat’s fur traps heat, not allowing it to escape into surrounding air to be detected by infrared camera. Credit: NASA/IPAC

Planets radiate mostly in the infrared, as do cool galactic gas clouds.  Certain wavelengths of infrared radiation has the ability to pass through dust clouds.  Thus, infrared observations can peer into dusty regions in space and see what lies behind the shroud of dust.  As a result, infrared astronomy is used for planetary observations, to detect protostars inside of nebulae, and to peer into the galactic center behind the wall of interstellar dust.  In other words, the form of radiation Herschel discovered is now used to better understand the very objects Herschel observed.

The video below is a montage of 2.5 million images of the Milky Way taken by the Spitzer Infrared Space Telescope.  As certain wavelengths of infrared are not absorbed by the interstellar medium as optical light is, the Spitzer images provide us with the true shape of our home galaxy including the central bulge that contains a massive black hole.

The Spitzer GLIMPSE360 website has an interactive where you can explore different regions of the Milky Way or select objects to view.  The Milky Way is not the only region that can be explored in infrared.  In 2014, the Keck Observatory imaged Uranus with infrared.

Images of Uranus, such as the ones taken by Voyager, tend to reveal a featureless planetary disk.  However, the Keck infrared image revealed storm activity to an extent not seen before on Uranus.  This might be indicative of an internal heat source that was not thought to exist previously on the gas giant.  Astronomers will need to revise current theories on the interior of Uranus as a result of this work.

Left-Uranus at 1.6 microns. White spots are storms below upper cloud layer. Right-Uranus as 2.2 microns. White spots are storm activity just below tropopause.  Uranus ring system is visible in this image. Credit: Imke de Pater (UC Berkeley) & W. M. Keck Observatory images.

As one would expect, many honors have been accorded upon the Herschel name.  This would include the 3.5 meter infrared Herschel Space Observatory and the 4.2 meter William Herschel Telescope in the Canary Islands.  However, the highest honor we can bestow upon William Herschel is the continued exploration of the celestial bodies he discovered, using the infrared radiation that he also discovered.

*Image on top of post, Sir William Herschel, by Lemuel Francis Abbott, oil on canvas, 1785, © National Portrait Gallery, London, Creative Commons License.

Mount Wilson – the Birthplace of Solar Physics

Perched 5,710 feet above the Los Angeles Basin in the San Gabriel Mountains, Mt. Wilson Observatory is noted for the ground breaking work of Edwin Hubble during the 1920’s.  In that decade, Hubble would discover galaxies beyond the Milky Way and the expansion of the universe at the observatory’s 100-inch telescope, then the world’s largest.  Located a few hundred feet from the famous telescope lies three solar telescopes whose observations provided the groundwork for our current understanding of the Sun.  This story did not begin in the warm climes of Southern California, but in the Upper Midwest at Yerkes Observatory, 90 miles northwest of Chicago.

The first director of Yerkes Observatory was George Ellery Hale.  The observatory, established in the 1890’s, is dubbed the birthplace of modern astrophysics.  Hale was the guiding force behind the building of the observatory and wanted to move astronomy from the study of the positions of celestial bodies in the night sky to the physics behind those objects.  Hale had an intense interest in the study of the Sun and set out to build a solar telescope on the grounds at Yerkes.  The result was the Snow Solar Telescope built in 1903.  The name of the telescope is not derived from Wisconsin winters, but from Helen Snow of Chicago who anted up $10,000 ($258,000 in 2014 dollars) to build it.  However, poor optical quality necessitated a move of the Snow from Wisconsin to California.

Driving down a highway on a hot summer day, you have probably seen heat waves rising from the ground and distorting your vision.  This effect is magnified if you attempt to take a picture through a telephoto lens.  The Snow Solar Telescope design had a movable mirror (coelostat) reflect the Sun’s image to a 30-inch mirror which in turn reflected the light 60 feet to 24-inch mirror that projected the final 6-inch image of the Sun.  Heats waves from the ground interfered with the image quality as the light traveled its 60 foot path horizontally to its final destination.  Hale thought relocating the Snow to an area with thinner air would reduce the heat interference problem.

As a result, the Snow was dismantled and transported to Mt. Wilson in California in 1904.  One does not normally associate the Los Angeles basin with good optics, but the summit of Mt. Wilson lies above the atmospheric inversion layer that traps the infamous Los Angeles smog like a lid on a pot.  This, combined with the thinner air of the higher altitude, improved the image quality of the Snow.  Hale set out to study sunspots, which would provide the first significant scientific finding from Mt. Wilson.

The Sun on July 28, 1906. Earth superimposed for scale. Credit: Mt. Wilson Observatory.

The oldest known observations of sunspots dates back to 800 B.C. both from ancient Chinese and Korean astronomers.  Historical recordings of sunspot numbers dates back to the 1600’s and constitute one of the longest ongoing scientific programs of observation.  At the dawn of the 1900’s, the nature of these spots on the Sun’s surface were not known.  Among the competing theories at the time were sunspots as debris clouds from solar tornadoes, areas hotter than the surrounding surface, and one of the most colorful ideas, sunspots as holes in a shroud of the Sun that hid a solid surface underneath.  The Snow Solar Telescope would begin the process to clarify the nature of sunspots.

The Snow was equipped with a high resolution spectrograph.  With this, Hale was able to record and compare spectra lines from regions of the Sun’s surface with and without sunspots.  These spectra lines were in turn compared to spectra produced in a laboratory under different temperature regimes.  In the cooler regime, many spectra lines were strengthened, and a few were weakened.  The spectra obtained from sunspots correlated with the spectra obtained in the laboratory in the cooler regime.  Hence, sunspots were regions on the solar surface that are cooler and thus, darker than the surrounding area.  The question remained, why were these regions cooler?  To answer this would require better solar images than the Snow could provide.

As George Ellery Hale was wont to do, he built a bigger and better telescope.  Despite the thinner air at Mt. Wilson, heat interference still proved to be an issue with the Snow.  To solve this, Hale built a telescope with a vertical, rather than horizontal design.  At 60-feet, the new solar tower was completed in 1908.  In his observations of sunspots, Hale was reminded how their structures were similar to the classic iron filings magnetic field experiments.  Based on this hunch, Hale set off to detect the presence of Zeeman lines in sunspot spectra.

60-foot Solar Tower (left) next to Snow Solar Telescope (right). Credit: Gregory Pijanowski
60-foot Solar Tower (left) next to Snow Solar Telescope (right). Credit: Gregory Pijanowski

The black lines seen in spectra are absorption lines.  Different elements absorb light at different wavelengths and this is how astronomers can figure out what stars, including the Sun, are made of.  If an atom absorbs light of the same energy as the difference between two electron orbital levels, the light energy is converted to energy that moves an electron to a higher orbit.  The result is the absorbed light creates a black line on a spectra.  The presence of a magnetic field creates more potential electron orbital levels.  As a consequence, a single absorption line can split into several absorption lines as can be seen below:

Credit: Astrophysics and Space Research Group, The University of Birmingham.

Using the new 60-foot solar tower, Hale was able to detect the presence of Zeeman lines in the spectra of sunspots.  In fact, the magnetic field in sunspots are several thousands times stronger than Earth’s magnetic field.  The intense magnetic fields in these areas of the Sun push plasma convection to areas outside of sunspot regions.  As it is this convection that transports heat to the solar surface, the magnetic blockage of this convection causes sunspots to be cooler by about 2,000 Celsius than the surrounding region.

Hale published this result in 1908six years after Zeeman won the Nobel Prize for his discovery of this effect.  This was the first time a magnetic field was discovered beyond Earth.  Hale would be nominated for a Nobel as a result of this discovery, but ultimately was not awarded.  Health issues eventually forced Hale away from Mt. Wilson, but not before building what would be the largest solar observatory from 1912 to 1962.

Mt. Wilson 150-foot Solar Tower. Photo: Gregory Pijanowski
Mt. Wilson 150-foot Solar Tower. Photo: Gregory Pijanowski

The 150-foot solar tower would be Hale’s last major contribution to solar astronomy.  The 150 foot vertical focal length produces a 17-inch image of the Sun at its base.  It was with this facility that Hale was able to determine the magnetic polarity of sunspots and the 22-year solar cycle.  The 11-year solar cycle had been long known and pertains to sunspot numbers only.  It usually takes 11 years (sometimes longer, sometimes shorter) for the solar cycle to reach one maximum to the next.

Magnetic fields are dipoles.  That is, a magnetic field will have a north and south pole.  Sunspots occur in pairs with one being the north pole and the other being the south pole, albeit at times a single spot in a pair will break up into several spots with the same polarity.  Hale discovered that sunspot pairs exhibit the opposite order of polarity in each solar hemisphere.  The polarities then reverse at the end of each 11-year cycle.  Consequently, a Hale 22-year solar cycle would look like this:

     Cycle (11-years)    Northern Hemisphere   Southern Hemisphere
                   1                        N-S                    S-N
                   2                        S-N                    N-S

The most recent occurrence of polarity reversal happened on January 4, 2008.  This event heralded the arrival of the current solar cycle.

By the mid-1920’s, Hale spent most of his time at his private solar observatory located in his residence in Pasadena.  He passed away in 1938 as work was ongoing for the 200-inch Mt. Palomar Observatory.  A new generation of solar astronomers would carry on his legacy at Mt. Wilson.

In 1957, Horace Babcock would install the first magnetograph in the 150-foot tower.  Rather than just study the strong magnetic fields of sunspots, the magnetograph was sensitive enough to map the magnetic field across the entire solar surface.  Essentially, the magnetograph maps the Zeeman effect across the entire solar disk.  Astronomers would take the work at the 150-foot tower a step further in the 1960’s by using it to study the Sun’s interior with a field called helioseismology.

In 1962, Robert Leighton discovered oscillations all across the solar surface which occurred in 5 minute cycles.  The theoretical modeling of these oscillations were refined by Roger Ulrich, who also kept the 150-foot Solar Tower in operation after the Carnegie Institution pulled their financial support in 1984.  These oscillations are caused by acoustic waves trapped inside the Sun.  Measurements of these waves allowed for modelling the solar interior.  One of the findings is the amount of hydrogen converted to helium in the solar core via fusion reactions.  This finding verified current models of solar evolution.  In other words, we know the Sun will be around for another 5 billion years or so.

The mapping of the solar magnetic field and helioseismology forms a key part of NASA’s current Solar Dynamics Observatory’s mission, as explained in the video below:

During the late 1990’s, I had the opportunity to go inside all three of the Mt. Wilson solar telescopes as a student in the observatory’s CUREA program.  The Snow was used primarily and I’ll never forget cleaning off the direct current switches, seemingly straight out of Frankenstein’s laboratory.  Also had encounters with both tarantulas and rattlesnakes.  In between those adventures, got to study the Sun’s spectrum (just as Hale did 90 years earlier), imaged the Moon at night, and gaze out over the cliff into Pasadena and the Rose Bowl.  The  60-foot solar tower had AC/DC blasting in the observation room, while the 150-foot tower had a visitor’s book signed by both Albert Einstein and Stephen Hawking.

Looking down the ladder on the 150-foot Solar Tower. Credit: Gregory Pijanowski
Looking down the ladder on the 150-foot Solar Tower. Credit: Gregory Pijanowski

Since then, there has been two recessions and a major financial crash.  The result has been cutbacks in funding and a need for the solar towers to reduce staff like many businesses have.  The Snow is still used by CUREA students every summer.  The 60-foot solar tower is run by USC.  The 150-foot tower had its funding shut down and is run on a volunteer basis.  The historic magnetograph made its last observation in 2013.  It could be much worse, in 2009, a forest fire came within a few hundred yards of the observatory which was saved by the efforts of several hundred firefighters.

Below is a video on the current effort to keep the 150-foot solar tower’s record of observations unbroken:

The observatory continues to reinvent itself.  The Pavilion, closed in the 1990’s, is now home to the popular Cosmic Cafe.  The grounds, once open to the public only on weekends is now open daily.  Public viewing is now offered on both the 60 and 100-inch telescopes.  The CHARA interferometer, which had started construction when I was there, is producing scientific results.  How do the solar towers fit in?  The 150-foot tower has been an important link in the continuous observations of sunspots since the early 1600’s.  In fact, those records compose 25% of that history.  And so far, it has been able to continue to do so.  I truly hope that chain is not broken.

*Image on top of post is the 60 and 150-foot towers keeping their vigil on the Sun.  Photo:  Gregory Pijanowski

To Catch a Star

Prior to the New Horizons flyby this month, the best image we had of Pluto came from the Hubble Space Telescope:
Credit: NASA, ESA, and M. Buie (Southwest Research Institute)

This struck me as being very similar to our best image of a stellar surface besides the Sun.  Very few stars have had their surfaces resolved.  Most stars appear as points of light in even the largest of telescopes.  Below is an image of Betelgeuse taken by the Hubble:

Credit: Andrea Dupree (Harvard-Smithsonian CfA), Ronald Gilliland (STScI), NASA and ESA

So the question to ask is, how can we obtain high resolution images of stellar disks as we did with Pluto?  Barring radical advancements in spacecraft propulsion, sending a mission to a star is not feasible.  The nearest star, Proxima Centauri, is 4.24 light years away from us.  The New Horizons probe, which is traveling at 35,000 mph (56,000 km/hr), would take over 100,000 years to reach that destination.  Obviously, the solution is constrained to be Earth bound or near Earth technology.  We need to build telescopes with higher resolution.

The theoretical resolution capability of a telescope is measured by the following equation:

R = 1.22(λ/d)

Where R is resolution in radians, λ is light wavelengths, and d is the diameter of the telescope’s primary mirror.  The smaller the value R, the higher the resolution and the greater the ability of a telescope to resolve finer detail.  Thus, to improve resolution, we’re gonna need a bigger telescope.

The other factor to consider is a telescope’s light gathering ability.  This is directly related to the area of the primary mirror.  If the mirror is circular in shape, this is described as:

A = πr2

Where A is area, π is the constant pi (about 3.14), and r is the radius of the mirror.  The larger A is, the larger a telescope’s ability to collect light.  Thus, a larger telescope can detect dimmer objects in the sky.  It can also detect objects farther away from Earth.  A mirror with a radius of 1 meter has an area of 3.14 square meters.  A mirror with a radius of 2 meters has an area of 12.56 square meters.  In other words, doubling the radius increases the area by four times.  Thus, what a mirror with a radius of 1 meter (diameter of 2 meters) can see 10 light years away, a mirror with a radius of 2 meters (diameter of 4 meters) can see 40 light years away.

To sum up the above, mirror diameter resolves finer detail on an object while surface area will enable more targets to be imaged.

As you might gather from the above, the best stellar targets to resolve would be stars that are very large (and hence, very bright) and relatively close.  And that is why Betelgeuse was the first star to be resolved in 1995 by the Hubble.  Betelgeuse is a red giant whose diameter could fit the orbit of Mars.  It is fairly close at 642 light years.  However, observing time is scarce on the Hubble as competition is fierce to use it.  Utilizing surface observatories can open up more opportunities for this line of research.

Besides the Hubble, another telescope to resolve a stellar disk is the CHARA array at Mt. Wilson.  CHARA relies on a technique referred to as interferometry.  An array of telescopes can have the same resolving ability of a single telescope the same size.  This is dependent upon the lightwaves received from all the telescopes in the array to be synced in phase together.

Credit: Mt. Wilson Institute

Radio astronomy was the first to use interferometry.  Radio waves are much larger than light waves.  In fact, radio waves can be several kilometers long.  Hence, it was easier to synch radio waves together than optical lightwaves.  The Very Large Array (VLA) in New Mexico uses this technique.  If you seen the movie Contact, you may be familiar with the VLA.  The VLA is an array of 27 radio antennas that in its widest configuration can provide the same resolution as a single antenna 22 miles (36 kilometers) wide.

Credit: Wikipedia/Hajor

Both economics and physics play a role here.  It is less expensive and structurally easier to build an array of small antennas rather than build a single dish 22 miles wide.  The tradeoff is gaining resolution at the cost of collecting ability.  The VLA does not collect the same amount of radio waves as a single 22 mile wide dish.  This plays a role in optical interferometry as well.

Optical interferometry presents a couple of challenges radio interferometry does not.  Visible light waves are disturbed by atmospheric turbulence, that is what causes the twinkling you see when you look at the stars at night.  The other is light waves are much smaller than radio waves.  In fact, radio waves are 1,000 – 1,000,000 times longer than visible light waves.  As a result, optical interferometry took longer than radio interferometry to develop.  Adaptive optics solved the turbulence problem.  Computer guided optical tracks solved the problem of combining very small visible light waves.

Credit: MRO/NMT

In the above example, light from the star travels a longer path to telescope 1 than to telescope 2.  Consequently, the light from telescope 2 must take an equally longer optical path before it is combined with the light from telescope 1 to ensure both are in phase together.  If the optical path is not calibrated correctly, the waves will arrive out of phase such as below:

Credit: Wiki Commons

The optical path is adjusted so that the red wavelength travels the distance θ longer than the optical path traveled by the blue wave so both waves are in synch and are combined where the peaks and valleys of the wave match up to produce a sharp image.

The CHARA interferometer currently has the longest baseline with six 1-meter telescopes spread out with a diameter of 330 meters.  The CHARA is located adjacent to the 100-inch telescope at Mt. Wilson where Edwin Hubble made his historic discovery of the expanding universe.

In 2007, the first resolved image of a disk from a near sun-like star was produced by the CHARA.  The star was Altair located 17 light years from Earth.  The image is below:

Credit: CHARA/GSU

Altair’s differs from the Sun in that its rotation rate is much faster.  The Sun rotates once every 25 days.  Altair rotates once every 9 hours.  Consequently, Altair is not spherical but bulges out from its equator.  This also causes Altair to have a cooler temperature at the equator and is thus darker in those regions.  This is the type of detail we can obtain when stars can be resolved as disks rather than points of light.

So what does the future hold?  Can future telescopes provide high resolution detail of stellar surfaces just as New Horizons provided for Pluto?  What should we hope to find if we can?  Stars, like planets, come in many sizes with differing physical characteristics.  The only star we can see with fine detail is the Sun.  The Solar Dynamics Observatory (SDO) images the Sun in both visible and ultraviolet light.  This video is an excellent overview of the solar surface detail provided by the SDO.

Given that attempts to resolve stars light years away from Earth is still in its nascent stage, it will be many years before we achieve that kind of quality imaging.  Nonetheless, there are promising developments that should improve our ability to acquire more detail of the features on stellar surfaces.

The first is a new generation of 30-40 meter telescopes set to go online in the 2020’s.  Combined with adaptive optics technology, they will have resolution on the order of 10-12 times that of the Hubble Space Telescope.  That, along with their immense light collecting ability, should improve the amount of suitable stellar targets to resolve.

The second, is the Magdalena Ridge Observatory Interferometer (MROI) in New Mexico.  The MROI will consist of an array of ten 1.4 meter telescopes with a maximum baseline of 1115 feet (340 meters).  The anticipated resolution will be 100 times that of the Hubble.  No definite timeline is given for completion of the MROI as it is a matter of obtaining funding to continue construction.  However, it is partially completed and hopefully will be up and running within ten years.

Credit: MROI

The next logical step is to build an optical interferometer in space.  Since 2000, NASA has been working on preliminary plans for the Stellar Imager (SI) mission.  The SI would consist of an array of 20-30 one meter mirrors with a baseline of 0.5 km (1,640 feet).  The array would be located in the Lagrange L2 point.  The L2 point is a gravitationally stable region 1.5 million km (1 million miles) from Earth.  This is also where the James Webb Space Telescope will reside a few years from now.

Credit: NASA/GSFC

Why should we endeavor to resolve stellar surfaces?  This is key to understanding the magnetic activity of a star and the stellar wind that emanates from the star towards orbiting planets.  These results can be integrated from the findings of exoplanet research.  Questions to be answered are, does the star generate space weather that could prevent life from forming on orbiting planets?  How strong a magnetic field does an orbiting planet require to protect life from local space weather conditions?  Does the star’s magnetic and irradiance cycle oscillate  in a manner that might inhibit the formation of life in its planetary system?  Detailed information from  main sequence stars older than the Sun could give us a look at the future of the Sun and how its evolution will impact life on Earth.

The SI is currently projected to start sometime around 2025-30.  More than likely, it will be later than that.  That is not unusual for cutting edge space missions.  The concept for an orbiting telescope was first proposed by Lionel Spitzer in 1946.  It took 44 more years to become reality as technical, funding, and political hurdles had to be overcome culminating with the launch of the Hubble Space Telescope in 1990.

I may never see the SI become reality in my lifetime, but it is important for my generation to lay down the ground work for our children to benefit from the results.  Astronomy, just like the building of the great cathedrals, can often be a multi-generational effort.

*Image on top of post are stars resolved by CHARA.  These stars are rapid rotators whose swift spinning motion flattens out their shape at the equator.  The images are false color and are designed to demonstrate temperature gradients on the surface of each star.  The brighter the color, the hotter the star is at that region.  The arrow on top indicates the true color of each star.  Credit:  CHARA/MIRC