Tuesday, July 22, 2014

Tropical Depression Two (2014)

Storm Active: July 21-23

On July 16, a tropical wave emerged off of the coast of Africa. A few days later, the system began to show signs of development, the first tropical wave of the season to do so. On July 20, shower and thunderstorm activity increased in association with a low pressure center forming along the wave. Despite being over the open central Atlantic, where sea surface temperatures were hardly sufficient for convective development, the low continued to organize the next day as concentrated thunderstorms appeared about the center. By the afternoon of July 21, it became evident that the low had acquired a closed circulation, and advisories were initiated on Tropical Depression Two.

On July 22, as the system proceeded westward under the influence of a subtropical ridge, dry air began to affect the system from the north, limiting the small amount of deep convection associated with Two primarily to the southern and western quadrants. The depression became slightly more organized that evening as thunderstorm activity increased briefly in coverage and intensity. However, by the morning of July 23, wind shear had also begun to increase, and the circulation started to lose definition due to the hostile atmospheric conditions. A few hours later, it became evident that the circulation was no longer closed, indicating that Tropical Depression Two had degenerated into a trough of low pressure.



As evident in this satellite image, Tropical Depression Two experienced an invasion of dry air from the north throughout its short lifetime.

Tuesday, July 1, 2014

Hurricane Arthur (2014)

Storm Active: June 30-July 5

On June 25, a frontal boundary oriented east to west over the northern United States began to push southward. Around June 27, a low pressure center formed along the front over North Carolina. Over the next day, the low drifted southeastward over South Carolina and emerged off of the coast early on June 28. Immediately, convection increased in association with the system.

In a region of weak steering currents, the low drifted slowly to the south, bringing rain showers to the northern Bahamas and eastern Florida by June 29. However, wind shear out of the north also increased that day, inhibiting the development of shower activity near the low's center. Despite this lack of convection, the low itself deepened significantly by June 30. Late in the day, upper-level winds once again became more favorable as wind shear dropped to near 10 kt. At this time, reconnaissance aircraft indicated that the system was just below the threshold of becoming a tropical cyclone. By just before midnight, organization had increased sufficiently to classify the system as Tropical Depression One, the first tropical cyclone of the 2014 Altantic Hurricane Season.

Tropical Depression One slowed and became nearly stationary off of the central Florida coast during the morning of July 1. Meanwhile, through the center of circulation remained on the northern edge of thunderstorm activity, banding and convective organization improved and the cyclone strengthened into Tropical Storm Arthur. Though the tropical storm reamined quite close to the U.S. East Coast, most of the deep convection was confined to the southern and eastern parts of the circulation, sparing land areas of the heaviest rain. Banding slowly improved throughout the day, indicating gradual strengthening By that evening, Arthur had begun a definite northward motion ahead of a trough moving into the southeastern United States. Central deep convection remained inconsistent into the morning of July 2, but the cyclone deepened and showed hints of an eye, and Arthur had soon intensified into a strong tropical storm.

Arthur persisted in its northerly motion throughout the day and most of the night, and meanwhile continued to strengthen. An eye feature made a brief appearance on visible satellite imagery during the afternoon of July 2, and the storm continued to gain in organization through the morning of July 3, even despite some ingestion of dry air from the north. By this time, rain bands had begun to sweep over the coasts of the Carolinas. Later in the morning, Arthur finally began to take its long anticipated eastward turn ahead of a front approaching the U.S. east coast and began to accelerate north-northeast.

That afternoon, Arthur developed a well-defined eye apparent on both visible and infrared imagery, indicating that another phase of strengthening was beginning. By the evening, the cyclone was upgraded to a category 2 hurricane. At 11:15 pm EDT on July 3, Hurricane Arthur made landfall near Cape Lookout, North Carolina, reaching its peak intensity of 100 mph winds and a minimum pressure of 973 mb, already stronger than any cyclone of the 2013 Atlantic hurricane season. Around 5:00 am on July 4, the center of circulation passed over the northern Outer Banks and emerged into the Atlantic. Meanwhile, the system's outer bands affected the coastal areas of Virginia, Maryland, Delaware, and New Jersey.

Increasing wind shear and colder waters began to weaken Arthur that morning, even as its windfield expanded, indicating that the extratropical transition had begun. Late on July 4, Arthur made its closest approach to Cape Cod as a minimal category 1 hurricane, bringing heavy rainfall and some tropical storm force winds to the region. By this time, Arthur was accelerating rapidly to the northeast and losing tropical characteristics. Early on June 5, the Arthur made landfall in southern Nova Scotia as the remaining deep convection became separated from the low-level center. The cyclone became post-tropical shortly afterward. The remnants of Arthur continued north and northeast over Newfoundland and into the North Atlantic near Greenland.



Hurricane Arthur was the first hurricane to make landfall in the United States since 2012.



Arthur took a rather unexpected shift to the west before landfall, bringing it inland over the Outer Banks of North Carolina.

Thursday, May 22, 2014

Professor Quibb's Picks - 2014

My personal predictions for the 2014 Atlantic hurricane season is (written May 22, 2014)

13 cyclones attaining tropical depression status,
12 cyclones attaining tropical storm status,
4 cyclones attaining hurricane status, and
1 cyclone attaining major hurricane status.

These predictions are near normal for the tropical depression and tropical storm categories, and below normal for the hurricane and major hurricane categories. The last 15 years have for the most part seen exceptionally high tropical cyclone activity due to the "warm" phase of the Altantic Multi-Decadal Oscillation (AMO). This oscillation (involving anomalies in sea surface temperatures) could explain the high tropical cyclone activity in the 1950's, the low activity in the 1980's, and the high activity in the 2000's. The current warm phase is expected to last at least several more years, likely keeping the number of tropical cyclones close to average even during seasons in which conditions are not generally favorable, such as this coming season.

ENSO oscillation forecasts indicate that an El Nino is likely to develop during the 2014 hurricane season, particularly in the late summer. Since an El Nino event is associated with a strong jet stream across the U.S. and higher wind shear, the development of such an event is likely to supress hurricane activity. Since the event is predicted to develop near the peak of the season, hurricanes and major hurricanes (which form more often near the peak of the season) are less likely.

In a manner similar to last season, the ocean temperatures of the east Atlantic are predicted to be below average for much of this season. This too discourages the formation of major hurricanes, since powerful tropical cyclones most often have their origins in the east Atlantic. During August 2013, a large quantity of Saharan dust was blown westward over the eastern Atlantic, cooling the water and disrupting cyclone formation. Though such events are difficult to forecast, above average trade winds could result in a similar event this season, further reducing eastern Atlantic activity.

Below, my anticipated risk factors for four major regions of the Atlantic basin are listed. The risk index runs from 1 meaning very low potential to 5 being very high potential (with 3 about average).

U.S. East Coast: 3
Though the season as a whole is expected to be inactive, any cyclones which do develop are likely to curve northward due to the position of the Bermuda high pressure system farther to the east during an El Nino. Thus the possibility exists for a grazing blow to coastal areas, especially Cape Hattaras.

U.S. Gulf Coast/Northern Mexico: 2
The Gulf of Mexico (particularly its northwestern section) have recorded persistently low sea surface temperature this year compared to the rest of the Atlantic basin. This factor, combined with the strong upper-level winds and powerful frontal boundaries passing over the U.S. Gulf coast, will likely destroy cyclones approaching the region.

Yucatan Peninsula and Central America: 2
This season, the upper atmospheric conditions favor cyclones paths which curve to the north, due to the eastward position of the Bermuda High pressure region. Usually, cyclones must take a more westward track without curavture in order to affect Central American regions and the Yucatan Peninsula. Any tropical systems reaching land therefore are likely to be weak tropical storms. In fact, this region is more at risk from Eastern Pacific tropical cylones than Atlantic ones.

Caribbean Islands: 2
During an El Nino season, Caribbean summers tend to be dry, due to a dry air mass situated over much of the region. In addition, persistent wind shear also pervades the Caribbean during an El Nino. The combination of these two factors can halt tropical cyclone development for weeks on end, ensuring that any storms that do develop pass to the north. The largest risk to the Caribbean Islands is for a cyclone to pass just to the north.

Overall, the 2014 Atlantic Hurricane Season is expected to be below average, particularly in intense cyclones, and the risk to most landmasses is smaller than normal. However, as history has repeatedly demonstrated, even quiet seasons may have devastating storms, such as Hurricane Andrew of 1992. Only 7 tropical storms formed that year, but one, Andrew, made landfall in Florida as a category 5 hurricane, only the third Atlantic hurricane to make landfall at such an intensity in recorded history. During any season, hurricane preparedness is a must.

Wednesday, May 14, 2014

Hurricane Names List-2014

For the North Atlantic Basin, the list for naming tropical cyclones in 2014 is as follows:

Arthur
Bertha
Cristobal
Dolly
Edouard
Fay
Gonzalo
Hanna
Isaias
Josephine
Kyle
Laura
Marco
Nana
Omar
Paulette
Rene
Sally
Teddy
Vicky
Wilfred

This list is the same as the 2008 list with the exception of Gonzalo, Isaias, and Paulette, which replaced Gustav, Ike, and Paloma, respectively. These names were retired after the 2008 season.

Wednesday, April 30, 2014

MAVEN

MAVEN (Mars Atmosphere and Volatile EvolutioN) is a NASA space mission primarily focused on studying the Martian atmosphere. Previous Mars missions have already given us hints into Mars's past, including numerous signs of past liquid water and various geographical and chemical signatures of a planet that was habitable many, many years ago. MAVEN will approach the problem of elucidating Mars's past from a different angle, by examination of its upper atmosphere.

Before MAVEN, our hypothesis as to the demise of Mars's habitability was as follows: several billion years ago, when the Solar System and its planets were still young, Mars had, like Earth, a molten core.



Earth's molten core consists of metals such as iron that conduct electricity. The circulation of these metals throughout the core, induced by the rotation of the Earth, generates a magnetic field (as in the illustration above). This magnetic field, in turn, protects us from the charged solar wind by deflecting it towards the poles. Mars is theorized to have had a similar core and magnetic field. However, being farther from the Sun and smaller, Mars's core cooled over time, and eventually solidified. The planet's magnetic field then weakened, and solar wind blew away a majority of Mars's atmosphere, leaving it with a rarefied layer of mostly carbon dioxide. Such a thin atmosphere would have been inhospitable for liquid water, and thus any bodies of water dried up, likely killing any life, if it had developed there.

MAVEN's observations will probably not alter this basic understanding, but will provide much more detailed information. For example, by observing how solar wind interacts with Mars's current atmosphere, the spacecraft will provide data concerning the exact mechanisms involved in atmospheric loss. To this end, MAVEN carries several instruments that measure solar wind and its impact on Mars. Also, by observing the current rate of gas loss, the mission will allow scientists to extrapolate backward and infer a more precise timeline of Mars's climate evolution. In order to accomplish this goal, MAVEN includes instruments that detect gaseous ions escaping from the Martian atmosphere. These are the "volatiles" to which the name refers. Finally, the probe also has a device known as a mass spectrometer, which can measure the abundance of different isotopes of certain chemical elements. Since heavier isotopes are less likely to be ejected from Mars simply due to their slightly greater mass, the ratio of isotope abundance in Mars's atmosphere versus that in Earth's, for example, can indicate exactly how much has been lost and thus how dense the atmosphere was in the past.

Artist's rendering of MAVEN

MAVEN launched on November 18, 2013. After about a ten month cruise, the probe will enter orbit of Mars in September of 2014. A few weeks after, the spacecraft will assume its science orbit, a highly elliptical orbit. The low point of its orbit brings MAVEN within 100 miles of the surface, allowing it to easily sample the atmosphere, and the high point brings it to more than 3000 miles from Mars's surface, so that the spacecraft can also take global observations. The science phase is planned to last about a year.

Sources: http://www.nasa.gov/mission_pages/maven/main/index.html#.Uf03vZIsmG0, http://www.nasa.gov/sites/default/files/files/MAVENFactSheet_Final20130610.pdf, http://lasp.colorado.edu/home/maven/science/, http://www.ipgp.fr/~aubert/Julien_Aubert,_Geodynamo,_IPG_Paris/Home.html

Wednesday, April 23, 2014

Eclipses and Saros Cycles 3

This is the third part of a three part post. To begin viewing the first, click here.

The previous post revealed the primary astronomical tool for predicting eclipses, the saros cycle. According to this cycle, the Moon has the same apparent size, inclination to the Earth's orbit, and angle to the Earth-Sun line in the Earth's orbital plane every 6585.32 days. Therefore, if an eclipse occurs on a given date, another very similar eclipse will occur about 18 years later with respect to the above parameters. During an eclipse, the angle of the Earth-Sun line to the Earth-Moon line will either be 0° (for a solar eclipse) or 180° (for a lunar eclipse), and the Moon will be at the same angle after a saros cycle, so two eclipses separated by a saros cycle must either both be solar or both be lunar. Similarly, during an eclipse, the Moon is either passing through the Earth's orbital plane at the ascending node or the descending node, and the eclipse after a saros cycle has passed will involve the Moon at the same node. Finally, the apparent size of the Moon will be the same for eclipses separated by a saros cycle.

However, many other conditions are not invariant before and after the length of time of a saros cycle. For example, since the decimal part of the length of the saros cycle is .32 days, two eclipses separated by a saros cycle will not be at the same time of day on Earth. In fact, the second eclipse will occur about 8 hours later than the first (.32 days is approximately 8 hours). This also guarantees that the eclipse will not occur in the same place on the Earth's surface. Futhermore, since the saros cycle is about 18 years and 11 days, the Earth will also be in two different places on its orbit around the Sun when the two eclipses occur.

In addition, 6585.32 days is not exactly an integral multiple of each of the synodic, draconic, and anomalistic months. For instance, 242 draconic months is about 6585.35 days (using the more precise value of 27.21222 days for the draconic month), which, although very close to the length of 223 synodic months, 6585.32 days, is not equal to it. As a result, even as as 223 synodic months pass from one eclipse and the Moon returns to its position along the Earth-Sun axis, the period of 242 draconic months is not quite complete, so the Moon will not have quite reached its node. Thus, over time, the eclipses separated by saros cycles shift until, eventually, the necessary conditions no longer align, and eclipses cease. Any given saros series will therefore only have a certain number of eclipses before the alignment ends.



The above image illustrates the progress of a saros series of lunar eclipses, where the gray bullseye represents the Earth's shadow (recall that if the Moon passes through the light gray, or partial shadow, of the Earth, the eclipse is partial, and if it passes entirely into the dark gray area, the total shadow, the eclipse is total). This series of eclipses is also at the descending node. Therefore, we can see that, before the saros series begins, the Moon has already passed the descending node at the time of the correct angular alignment of the Moon, Earth, and Sun. Thus the Moon is "too low" to be hit by Earth's shadow (blue-gray Moon). However, after a saros cycle has passed, the angular alignment is once again correct, but a full draconic month has not yet passed, so the Moon is a little less past its descending node than before.

Eventually, the draconic month has drifted backward enough so that the passage through the descending node does coincide with the correct arrangement of the Moon, Earth, and Sun in the orbital plane, and the path of the Moon does take it through the Earth's shadow. At this point, partial and then total eclipses will occur. However, over time, the Moon's progress in the draconic month will again fall behind, and at the time of correct angular orientation, the Moon will have not yet reached the descending node. At this point (the pink Moon), eclipses will cease and the saros series ends.



A similar phenomenon occurs with solar eclipses. In the above diagram, a few total solar eclipse paths across the Earth are shown, all from the same saros series (though there are many others), and again at the Moon's descending node. Note that each eclipse is indicated by a path along the Earth's surface. The paths are the areas which experience totality some time during the eclipse. The path of the eclipse moves from west to east, even though the part of the Earth facing the Sun moves from east to west along the globe. This is because the Moon's velocity, and thus the velocity of its shadow, is greater from west to east then the area that of the point on the Earth's surface moving from east to west.

As mentioned above, successive eclipses in a saros cycle are separated (in time of day) by about 8 hours, approximately a third of a day. Thus the second eclipse takes place about 120° west of the first. Thus two eclipses in a saros series three saros cycles apart will be at about the same longitude. But for the above series, which take place at the Moon's descending node, eclipses later in the series are not as far along with respect to the draconic month as those at the beginning. Thus, just as for lunar eclipses, the eclipses in a series at the descending node shift "upward", and in the solar case, this has the effect of shifting the totality path north for each successive saros cycle. Thus the first eclipses in the same saros series as above, are only partial, and can only be seen near the south pole. Eventually, as the series progresses, the Moon's shadow intersects the Earth, again beginning at low latitudes. As in the figure, the path shifts north until the eclipses can only be seen near the north pole, and then not at all. The down-to-up or south-to-north pattern for saros series reverses for series at the ascending node.

Saros series are numbered, with separate numberings for lunar and solar eclipse series. For lunar eclipses, those at the descending node are given odd numbers and those at the ascending node even numbers. The situation is reversed for solar eclipses. The saros series, further, are ordered in number by starting date. Contemporary series which are currently producing total eclipses are in the low to mid 100's. For example, the solar eclipse on August 21, 2017 belongs to solar saros 145. Solar and lunar saros series each include around 70 eclipse events, spanning a period of roughly 1200 years. Of course, these series overlap, so any given year, eclipses occur from different saros series. For example, the year 2012 had solar eclipses from series 128 and 133, while it had lunar eclipses from series 140 and 145.

In conclusion, saros series are the most important tool in the categorization of eclipses, and have allowed us to identify when eclipses have occurred thousands of years into the past, and to predict when the will occur thousands of years into the future.

Sources: http://en.wikipedia.org/wiki/Saros_(astronomy), http://www.cropcircleconnector.com/inter2012/italy/bracciano-earthquake7.jpg, http://www.math.nus.edu.sg/aslaksen/gem-projects/hm/0304-1-08-eclipse/Path%20of%20Totality.htm, http://eclipse.gsfc.nasa.gov/SEsaros/SEperiodicity.html#section106

Tuesday, April 15, 2014

Eclipses and Saros Cycles 2

This is the second part of a post concerning eclipses and saros cycles. For the first, see here.

To understand how solar eclipses are predicted, we first must define some terminology relating to various types of "months". These months are not calendar months, but rather are time intervals related to the moon's orbit.

Synodic Month (29.53 days): This is the most common period referenced in the context of the moon. It measures the time it takes for the Moon to complete a revolution with respect to the line between the Earth and the Sun, or the time between two full moons or two new moons. However, this month is not equal to the period of the Moon's orbit, because the line between the Earth and the Sun shifts, as the Earth itself revolves.



The above image shows the position of the Earth and the Moon relative to the Sun at two successive new moons. Note the angle between the line connecting the Earth and Sun and the line marking the point at which the Moon has completed exactly one orbit around the Earth. Such an orbit takes 27.32 days.

Draconic Month (27.21 days): This "month" is the average time between successive crossings of the ascending node by the Moon on its orbit. The nodes of an orbit are the orbit's intersection with some plane of reference. In the context of eclipses, we are concerned with the intersection of the Moon's orbit around the Earth with the plane containing the Earth's orbit and the Sun. Since the Moon's orbit is inclined to this plane, there are only two points of intersection (see diagram below).



The two nodes of the Moon's orbit are the ascending node, at which point the Moon crosses from below the plane of the Earth's orbit to above (where the area "above" the plane is the space beyond the Earth's north pole), and the descending node, where the opposite occurs. Since, due to the effect of the Sun's gravity, the nodes of the Moon's orbit shift with time against the Moon's direction of orbit, the draconic month (time between crossing ascending node twice) is slightly shorter than the orbital period of the Moon (27.32 days). The draconic month is important for the prediction of eclipses because eclipses can only occur when the Moon is in the plane of the Earth's orbit and the Sun, i.e., when the Moon is at an ascending or descending node.

Anomalistic Month (27.55 days): The Moon's orbit, just like the Earth's and that of other celestial bodies, is not a perfect circle. Thus the Moon's distance from Earth varies. The farthest point of the Moon's orbit from the Earth is known as the apogee (deriving from Ancient Greek "from" and "earth", the second of which also gives us geography, geocentric, etc.), and the closest point the perigee (with "peri" meaning "around").

Diagram of the Moon's orbit (elongation exaggerated)

The anomalistic month measures the time it takes for the Moon to travel from one apogee (or perigee) to the next. Note that this length of time is slightly longer than a lunar orbital period, because the apogee and perigee move along the lunar orbit in the same direction as the Moon's motion, so it takes longer for the Moon to "catch up" to its apogee than for the Moon to simply complete an orbit. The anomalistic month is important for eclipse prediction, because although it does not affect the apparent position of the Moon in the sky, whether the Moon is closer to apogee or perigee does affect its apparent size, and thus can affect the type and duration of an eclipse.

Apparent size of the Moon at apogee and perigee.

Note that the apparent size of the Sun varies too, as the Earth's orbit is also elliptical, but the variation occurs at only a fraction of the magnitude (about 3% variation versus the Moon's 12%). Therefore, we focus on the Moon's apparent angular diameter as the determining factor.

In summary, progress through the synodic month indicates the Moon's position relative to the Earth-Sun line (in the Earth-Sun orbital plane), progress through the draconic month indicates how far the Moon is from the Earth-Sun orbital plane, and progress through the anomalistic month indicates the Moon's apparent size. It so happens that the length of time equal to 223 synodic months is about the same as that of 242 draconic months and 239 anomalistic months, all of which equal approximately 6585.32 days. The reason this is significant is that after this period of time passes, a whole number multiple of each of the three "months" will have passed, and the Moon will be in almost exactly the same position relative to the Sun, the same apparent size, and the same inclination from the Earth-Sun orbital plane. Thus if an eclipse occurs at a given date, a nearly identical eclipse will occur again 6585.32 days later! A period of 6585.32 days, about 18 years, is known as a saros cycle.

The sequence of eclipses produced beginning at a given date and including all the eclipses separated from the first by some number of saros cycles is known as a saros series. Eclipses, both lunar and solar, are classified by saros series. The next post explores the details and applications of saros cycles and series.

Sources: http://www.hermit.org/eclipse/Graphics/diagrams/Rotations3.png, http://en.wikipedia.org/wiki/Saros_(astronomy), http://www.hermit.org/eclipse/Graphics/diagrams/Draconic.png, http://www.metahistory.org/images/moonorbit.gif, http://www.astro.virginia.edu/class/whittle/astr1230/im/moon_sidereal.gif

Monday, April 7, 2014

Eclipses and Saros Cycles 1

Solar and lunar eclipses are among the most spectacular of celestial phenomena. One of the great triumphs of astronomy was the accurate prediction of solar eclipses, beginning with Ancient Greek and Chinese astronomers. These predictions depend on a study of the cycles of the Earth, the Moon, and the Sun, known as Saros Cycles.

First, however, an explanation for the mechanism of eclipses is in order. A eclipse occurs when the Sun, the Moon, and the Earth are in a straight line, so that the Moon casts a shadow on the Earth, or vice versa. When the Earth casts a shadow on the Moon, the eclipse is lunar. When the Moon casts a shadow on the Earth, the eclipse is solar. An illustration of both of these eclipse types is shown below (not to scale).



In a solar eclipse, only a very small portion of the Earth's surface receives the shadow of the Moon, and this shadow moves across the Earth's surface as the Moon moves along its orbit. Furthermore, from the viewpoint of the observer on Earth, a solar eclipse is total when one is within the shadow of the Moon, and partial when one is in the partial shadow of the Moon (see above figure). The dark gray area is the shadow of the Moon, where both sides of the Sun are invisible. Thus in a total solar eclipse, none of the Sun is visible.

Total Solar Eclipse

The light gray area in the above diagram is the partial shadow, or penumbra. In this region, one side of the Sun is visible, but the other is blocked from view. In a partial solar eclipse, the Sun is never completely covered by the Moon, but the Moon rather skirts the Sun, covering only one of its edges.

Partial Solar Eclipse

Note that, on the diagram, since the Sun is larger than the Moon, the rays of the Sun on either side of the Moon converge with distance, and the shadow of the Moon on the Earth is a great deal smaller than the Moon itself. In fact, since the distance between the Earth and the Moon varies, when the Moon is farthest from the Earth and an eclipse occurs, the shadow of the Moon no longer reaches the Earth. In other words, from the perspective of the Earth viewer, the size of the Moon's disc is smaller than the size of the Sun's disc, and the Moon cannot cover the Sun. This leads to a phenomenon known as a annular solar eclipse.

Annular Solar Eclipse

Conversely, a lunar eclipse occurs when the Earth is between the Sun and the Moon. There are partial and total lunar eclipses as well, although the definitions differ slightly, as they are geocentric; in other words, the definitions are not based on an observer on the Moon, rather one on the Earth. Since the Earth's shadow is large, it can completely cover the Moon, as opposed to a solar eclipse, which is a localized event. A partial lunar eclipse is one in which the Earth's shadow does not completely cover the Moon, and a total lunar eclipse is one in which the Earth's shadow completely covers the Moon. During a total lunar eclipse, the Moon takes on a characteristic red color.

Total Lunar Eclipse

The Moon appears red during a lunar eclipse due to the fact that the only light reaching the Moon passes through a good deal of the Earth's atmosphere. Most short wavelengths of light are scattered by the time the Sun's rays have passed all the way through, so only long-wavelength light remains, causing the Moon to appear red in the visible spectrum. The same effect makes sunrises and sunsets appear red.

Though these types of solar and lunar eclipses differ in appearance, they are all manifestations of the same phenomenon: the alignment of the Sun and the Moon with respect to the Earth. Looking only at the diagram of a solar eclipse, one would believe that such events would be quite common, and would occur every time the Moon orbits around the Earth to come in line with the Sun. This would be true if the orbits of the Sun and the Moon lay in the same plane. However, the plane of the Moon's orbit around the Earth is inclined relative to the plane of the Earth's orbit around the Sun, and to make matters worse, the orbit is constantly shifting.

The next post discusses how eclipses can be predicted by understanding the various cycles of the Moon, Earth, and Sun.

Sources: http://eclipse.gsfc.nasa.gov/eclipse.html, http://image.gsfc.nasa.gov/poetry/ask/a11846.html, http://kids.britannica.com/elementary/art-87433/During-a-solar-eclipse-the-Moon-passes-between-the-sun, http://indiancountrytodaymedianetwork.com/sites/default/files/uploads/2012/11/solar-eclipse.jpg, http://www.topnews.in/files/SolarEclipse.jpg, http://upload.wikimedia.org/wikipedia/commons/thumb/3/37/Annular_Eclipse._Taken_from_Middlegate,_Nevada_on_May_20,_2012.jpg/320px-Annular_Eclipse._Taken_from_Middlegate,_Nevada_on_May_20,_2012.jpg, http://en.wikipedia.org/wiki/Saros_(astronomy),

Sunday, March 30, 2014

Gravitational Waves 2

This is the second part of a two-part post on gravitational waves. For the first part, see here.

The previous post introduces gravitational waves, and discusses early attempts at their detection, such as LIGO. Despite LIGO's failure to detect these waves, new instruments promise to increase precision, allowing us to find weaker gravitational waves, and other indirect methods have yielded results. Overall, these techniques will give us new methods of observing our Universe.

LIGO, as well as other early laser interferometer observatories such as VIRGO (a similar detector in Italy), are sometimes known as the "first generation" of gravitational wave detectors. During LIGO's operation, upgrades led to modest increases in sensitivity. However, after the temporary cessation of operations in 2010, more major upgrades were made to LIGO including heavier mirrors and more powerful lasers, which will increase sensitivity and reduce background noise caused by thermal energy. The new Advanced LIGO is scheduled to begin operation in 2016, and should have a range of hundreds of millions of light years, ten times that of the original design (see diagram below). These upgraded observatories will be the "second generation" of detectors.



The original LIGO could detect gravitational wave sources only within our Local supercluster and its neighbors (small gray sphere), but Advanced LIGO should be able to scour an volume of space 1000 times as large for gravitational wave signals (the entire scope of the figure above).



The above diagram shows the actual and estimated sensitivities for different gravitational wave detectors, including LIGO, VIRGO, and their planned respective upgrades. The x-axis of the graph is the frequency of the gravitational wave (gravitational waves have different frequencies in the same way that electromagnetic waves do) and the y-axis indicates the intensity of the waves. The detectors exhibit different sensitivities to different frequencies; curves that dip lower indicate better detectors. The Einstein GW Telescope is a proposed "third-generation" laser interferometer concept, still in design phase. This design would have the facility be underground to reduce seismic noise and cryogenically cooled to prevent thermal vibrations from altering the distance between mirrors.

Another "third-generation" design concept which would theoretically yield numerous detections is the Laser Interferometer Space Antenna (LISA), a spaced-based model.



LISA would consist of three separate spacecraft, which would create a equilateral triangle of side length 5 million kilometers (3.1 million miles). The above diagram is an artist's conception. This triangle would trail the Earth in heliocentric orbit, and would be very sensitive to different frequencies of gravitational waves than ground-based detectors like LIGO.



The above figure shows that LISA would detect much longer wavelengths than Advanced LIGO (due to LISA's enormous arms). Advanced LIGO could only discover very high frequency oscillations, such as neutron stars rotating very close to each other just before colliding. Such systems are rare and short-lived, since neutron star systems contract and ultimately collide. However, LISA could detect more slowly orbiting binary systems, long before their final collision. These are very common, and many are already known through other means of observation, guaranteeing that LISA would find many sources if it functions correctly.

There are unfortunately no definite plans for launching LISA, but a small test mission, known as LISA Pathfinder, is set to launch in 2015. This small probe contains a tiny interferometer meant to test the LISA concept in space and evaluate the proposal's feasibility.

Ultimately, the most important goal of gravitational-wave observatories is to peer farther into the early universe than could be possible with telescopes measuring electromagnetic radiation. Using ordinary visual telescopes (of sufficient power), we can view objects billions of light years away (seeing them as they were billions of years ago, since it takes light a year to travel each light-year). However, there is a fundamental limit to how far these telescopes can see. Before 380,000 years after the Big Bang (or about 13.8 billion years ago), the temperature of the Universe was too high for electrons to combine with atomic nuclei into atoms, and, since electrons scatter electromagnetic radiation, the Universe was opaque. Thus the "oldest" light in the Universe is from 380,000 years after the Big Bang; it is called the Cosmic Microwave Background (CMB), and traditional telescopes cannot see farther. However, gravitational wave astronomy has the potential to receive signals from earlier periods and study them directly, leading to a greater understanding of the Big Bang.

Despite the dearth of results from observatories thus far, other methods have found success. On March 17, 2014, scientists announced that the BICEP2 (Background Imaging of Cosmic Extragalactic Polarization 2) array, located near the south pole in Antarctica, had finally seen evidence of gravitational waves. They found that the CMB had been polarized, or twisted in a certain direction of oscillation, after its emission 380,000 years after the Big Bang. The culprit of this polarization, they announced, was gravitational waves. The specific way in which the waves distort space would have a polarizing effect on the light.

This remarkable discovery is still until scrutiny and awaiting independent verification, and it does much more than simply confirm the existence of gravitational waves (though this confirmation is important as another affirmation of Einstein's general relativity). The polarization provides important evidence for the theory of inflation in the early universe.



Many astrophysicists have subscribed to the theory of inflation, namely the theory that the Universe went into a period of exceptionally rapid expansion beginning about a trillionth of a trillionth of a trillionth of a second (10-36 seconds) after the Big Bang. The BICEP2 team's findings support this view of the Universe because inflation would have amplified tiny gravitational variations in the early Universe to waves large enough to polarize the CMB to the extent observed. The diagram above illustrates this idea: without inflation (left), gravitational waves would not have been amplified to the point of being detectable. However, an inflationary model predicts large gravitational ripples following the period of inflation (right), which would polarize the CMB many years afterward.

This discovery exemplifies what we hope to learn from gravitational waves. By observing these subtle oscillations of space, we may probe areas (and time periods) of the Universe inaccessible to traditional astronomy. We may even learn more about the beginning of our Universe.

Sources: https://www.advancedligo.mit.edu/summary.html, http://www.ligo.caltech.edu/docs/G/G080303-00.pdf, http://www.et-gw.eu/, http://www.physik.hu-berlin.de/qom/research/freqref/lisa, http://lisa.nasa.gov/, http://cosmology.berkeley.edu/~yuki/CMBpol/CMBpol.htm, http://www.theguardian.com/science/2014/mar/17/primordial-gravitational-wave-discovery-physics-bicep, http://www.nytimes.com/2014/03/25/science/space/ripples-from-the-big-bang.html?_r=0, "An Ear to the Big Bang" from The Scientific American October 2013 issue

Saturday, March 22, 2014

Gravitational Waves 1

Gravitational waves, in brief, are the propagations of gravitational fields through space. Before dealing with gravitational waves directly, we attempt to provide historical context and a way to visualize how the waves work.

In 1865, James Clerk Maxwell (1831-1879) published a paper outlining his theory of electromagnetism, compiling and uniting earlier work into a single theory explaining the properties of both electricity and magnetism. For example, it deals with the properties objects possessing positive and negative charges, and the forces they exert on their environments (electric and magnetic fields). This theory also describes electromagnetic waves, or propagating changes in the electromagnetic field. Such waves are characterized by their wavelength and amplitude.



The above simplified diagram of a wave shows its wavelength and amplitude. We also define the frequency of a wave as the number of oscillations per second. In the diagram above, the wave has a frequency of 2 Hz. For electromagnetic waves, amplitude corresponds to intensity of the wave, and wavelength to type (or in the case of visual light, color). The continuous interval of electromagnetic wavelengths is known as the electromagnetic spectrum and includes many familiar types of radiation, including radio waves, microwaves, infrared rays, visible light, ultraviolet rays, X-rays, and gamma rays (all of these types are discussed in the link above).

Such waves are produced when charged objects move through space, causing a change in electric field. When a charge has moved, it will not exert the same forces on its surroundings as it had previously. The change in field is "carried" by waves, which move at the speed of light, a finite (though very fast) speed. The diagram below shows an example of electromagnetic wave production by a dipole, or a pair of equal and opposite charges.



As the charges oscillate up and down, an electromagnetic wave is produced, and propagates away from the dipole (the blue and red parts of the oscillation are the electric and magnetic field components, respectively). Since the oscillation is periodic, the wave signal it produces is also periodic. The magnitude of the charges forming the dipole determines the amplitude of the generated wave. Also, the frequency of the oscillation determines the frequency of the electromagnetic waves.

At the beginning 20th century, though Maxwell's theory had supplanted earlier understandings of electromagnetism, Newton's was still the dominant paradigm for gravitation. The theories did have similarities, among them the fact that both electromagnetic and gravitational forces shrank with distance in inverse proportion with the square of this distance (F ~ 1/r2). However, while there were both attractive and repulsive electromagnetic forces, gravity was always an attractive force. Another crucial difference was that, as shown above, electromagnetic fields move at the speed of light. Newton's theory, though, simply assumed that all bodies pulled instantaneously on one another. Albert Einstein (1879-1955) developed the theory of general relativity in 1916 and resolved this difference. His theory predicted that differences in gravitational fields would move analogously to electromagnetic fields: using gravitational waves. Further, these postulated gravitational waves would travel at the speed of light.



Gravitational waves, in Einstein's theory, would also be produced in an analogous manner to electromagnetic waves. Instead of oscillating charges, oscillating masses would produce the waves. For example, two massive bodies (such as black holes) orbiting one another at close range would produce gravitational radiation, as in the diagram below.



The conception above illustrates how gravitational waves move away from the orbiting system in all directions. Unlike their electromagnetic counterparts, gravitational waves travel undisturbed through matter, and as a consequence are much more difficult to detect. Nevertheless, they do have a subtle effect on the matter which they pass through. The medium through which gravitational waves travel is the fabric of space itself. The diagram above illustrates distortions of a two-dimensional space fabric; in reality, gravitational waves would cause small "ripples" in our three-dimensional space.

Beginning in the 1960's scientists on Earth have constructed increasingly sophisticated gravitational wave detectors. The first variety were known as Weber bars, or large bars of metal which, if sufficiently isolated from the surrounding environment, could oscllate as gravitational waves passed through them. However, the waves had to be very strong to be detected, and the original models were not up to the task. More modern Weber bars have been supercooled to temperatures very near absolute zero to reduce outside vibrations and increase their sensitivity.

Another method for identifying incoming gravitational waves is known as laser interferometry.



Laser interferometry works by using light beams to measure distances. In the usual design (diagram above), a laser creates a beam of light which is split by a beam-splitting mirror into two beams which travel down the two perpendicular arms of the interferometer. On the return trip, if the arms are exactly the same length, the beams interfere with one another in such a way that all the light travels back to the laser. If, however, the arms have slightly different lengths, some light will be reflected by the beam-splitter into a detector.

The Laser Interferometer Gravitational-Wave Observatory (LIGO) wass one project making use of a laser interferometer to detect gravitational waves. In each of LIGO's facilities (there is one in Louisiana and one in Washington) there was a laser inteferometer with arms four kilometers (2.5 miles) long. Theory held that when a gravitational wave passes through the detector, it distorts space and actually alters the lengths of the arms slightly. Since the arms are perpendicular, the distortions are different, and sufficiently strong waves should then cause the laser beams to be enough out of sync to send light to the detector. There were two LIGO stations to weed out false data and to determine which way gravitational waves moved through the Earth. Despite the precision of LIGO, it did not make any unambiguous detections during its operation (2002-2010).

Despite these setbacks, concepts for more precise instruments and new detectors have since been developed, and the road to gravitational wave detection has also proceeded through more indirect means (see the next post, coming March 30).

Sources: http://www.britannica.com/EBchecked/topic/242499/gravity-wave, http://rsta.royalsocietypublishing.org/content/366/1871/1849.full, http://www.tapir.caltech.edu/~teviet/Waves/differences.html, http://www.geo.mtu.edu/~scarn/teaching/GE4250/EM_wave_lecture.pdf, http://ned.ipac.caltech.edu/level5/ESSAYS/Boughn/figure1.gif, http://upload.wikimedia.org/wikipedia/commons/3/35/Onde_electromagnetique.svg, http://www.vias.org/wirelessnetw/img/wndw-print_img_3.png, spaceplace.nasa.gov, http://en.wikipedia.org/wiki/Gravitational-wave_detector, http://www.learner.org/courses/physics/visual/visual.html?shortname=ligo_interfermometer, http://www.ligo-la.caltech.edu/LLO/overviewsci.htm