Capella OnlineOctober 2017 Edition
Welcome to the October edition of this newsletter.
The observing night in September turned out to be a clear and productive one with many objects viewed on the night and a successful set up of Winnie’s new mount and scope.
This month’s observing night will be on either 13th October depending on the weather.
The next practical workshop is scheduled for Wednesday 18th October. This and any other events are listed on the NSAS Events page.
The date for Stargazing at Millennium Green (Audley) is October 28th 2017 (6pm–9pm). More details here
If anyone wants to come along to help or bring scopes then please see me at the meeting or email email@example.com
NSAS Calendar 2018
If you have any astronomical images for inclusion in the 2018 calendar then please email to firstname.lastname@example.org
May I remind everyone that the society solar scope is available throughout the winter too! It is on a monthly basis and there is just a £25 returnable deposit required. Contact me at the email below or see me at the meeting. More details here.
If anyone has any ideas for new features on the website or on any improvements you’d like to see to existing ones then please drop me an email or text.
Also keep an eye on our Facebook page as any breaking news will more than likely appear there first as I can update that from my phone.
Our new members Facebook group is here
The sky maps can be downloaded from here
The next regular meeting is on November 7th , which is Mark Townley – ‘Our Local Star’
If anyone has anything they want to include on the website/newsletter/etc then please email me email@example.com
Wishing you clear skies, Duncan
Members Area access for this month (see email)
Sky Calendar — October 2017
|3||Moon near Neptune (152° from Sun, evening sky) at 12h UT. Mag. 7.8. Occultation visible from Tasmania and New Zealand.
• Occultation of Neptune (IOTA)
|5||Venus 0.2° NNE of Mars (23° from Sun, morning sky) at 17h UT. Mags. −3.9 and 1.8.|
|5||Full Moon at 18:41 UT.|
|8||Mercury at superior conjunction with the Sun at 21h UT. The elusive planet passes into the evening sky.|
|9||Moon near the Pleiades (morning sky) at 2h UT.
• The Pleiades (Wikipedia)
|9||Moon at perigee (closest to Earth) at 5:53 UT (366,855 km; angular size 32.6′).|
|9||Moon near Aldebaran (126° from Sun, morning sky) at 18h UT. Occultation visible from Asia.
• Occultation of Aldebaran (IOTA)
|12||Last Quarter Moon at 12:26 UT.|
|13||Moon near Beehive cluster (morning sky) at 20h UT.
• Beehive Cluster (Wikipedia)
• M44: The Beehive Cluster (APOD)
|15||Moon near Regulus (52° from Sun, morning sky) at 11h UT. Occultation visible from USA and Mexico.
• Occultation of Regulus (IOTA)
|17||Moon near Mars (28° from Sun, morning sky) at 11h UT. Mag. 1.8.|
|18||Moon near Venus (20° from Sun, morning sky) at 2h UT. Mag. −3.9.|
|19||Uranus at opposition at 17h UT. Mag. 5.7.|
|19||New Moon at 19:12 UT. Start of lunation 1173.
• Lunation Number (Wikipedia)
|21||Orionid meteor shower peaks. Arises from the debris field of Comet Halley. Active from October 2 to November 7. Produces very fast (66 km/sec), generally faint meteors (20 per hour). Radiant located near Orion’s club asterism. Observe after midnight on night of 21/22.
• Orionids (Gary Kronk)
• Meteor Shower Calendar (IMO)
|23||Moon near Antares (evening sky) at 8h UT.
• Antares (Wikipedia)
|24||Moon near Saturn (evening sky) at 12h UT. Mag. 0.5.
• Saturn (Wikipedia)
|25||Moon at apogee (farthest from Earth) at 2h UT (distance 405,154 km; angular size 29.5′).|
|26||Jupiter at conjunction with the Sun at 18h UT. Passes into the morning sky (not visible).|
|27||First Quarter Moon at 22:22 UT.|
|30||Moon near Neptune (124° from Sun, evening sky) at 21h UT. Mag. 7.8. Occultation visible from southern Africa.
• Occultation of Neptune (IOTA)
CONSTELLATION OF THE MONTH
|Symbolism||the Winged Horse|
|Right ascension||21h 12.6m to 00h 14.6m|
|Declination||+2.33° to +36.61°|
|Area||1121 sq. deg. (7th)|
|Main stars||9, 17|
|Stars with planets||12|
|Stars brighter than 3.00m||5|
|Stars within 10.00 pc (32.62 ly)||3|
|Brightest star||ε Peg (Enif) (2.38m)|
|Meteor showers||July Pegasids|
|Visible at latitudes between +90° and −60°.
Best visible at 21:00 (9 p.m.) during the month of October.
Pegasus is a constellation in the northern sky, named after the winged horse Pegasus in Greek mythology. It was one of the 48 constellations listed by the 2nd-century astronomer Ptolemy, and is one of the 88 constellations recognised today.
With an apparent magnitude varying between 2.37 and 2.45, the brightest star in Pegasus is the orange supergiant Epsilon Pegasi, also known as Enif, which marks the horse’s muzzle. Alpha (Markab), Beta (Scheat), and Gamma (Algenib), together with Alpha Andromedae (Alpheratz, once also designated Delta Pegasi) form the large asterism known as the Square of Pegasus. Twelve star systems have been found to have exoplanets. 51 Pegasi was the first Sun-like star discovered to have an exoplanet companion.
The Babylonian constellation IKU (field) had four stars of which three were later part of the Greek constellation Hippos (Pegasus). Pegasus, in Greek mythology, was a winged horse with magical powers. One myth regarding his powers says that his hooves dug out a spring, Hippocrene, which blessed those who drank its water with the ability to write poetry. Pegasus was the one who delivered Medusa‘s head to Polydectes, after which he travelled to Mount Olympus in order to be the bearer of thunder and lightning for Zeus. Eventually, he became the horse to Bellerophon, who was asked to kill the Chimera and succeeded with the help of Athena and Pegasus. Despite this success, after the death of his children, Bellerophon asked Pegasus to take him to Mount Olympus. Though Pegasus agreed, he plummeted back to Earth after Zeus either threw a thunderbolt at him or made Pegasus buck him off. In ancient Persia, Pegasus was depicted by al-Sufi as a complete horse facing east, unlike most other uranographers, who had depicted Pegasus as half of a horse, rising out of the ocean. In al-Sufi’s depiction, Pegasus’s head is made up of the stars of Lacerta the lizard. Its right foreleg is represented by β Peg and its left foreleg is represented by η Peg, μ Peg, and λ Peg; its hind legs are marked by 9 Peg. The back is represented by π Peg and μ Cyg, and the belly is represented by ι Peg and κ Peg.
In Chinese astronomy, the modern constellation of Pegasus lies in The Black Tortoise of the north (北方玄武), where the stars were classified in several separate asterisms of stars. Epsilon and Theta Pegasi are joined with Alpha Aquarii to form Wei 危 “rooftop”, with Theta forming the roof apex.
For the Warrau and Arawak peoples in Guyana the stars in the Great Square, corresponding to parts of Pegasus and of Andromeda, represented a barbecue, taken up to the sky by the seven hunters of the myth of Siritjo.
Covering 1121 square degrees, Pegasus is the seventh-largest of the 88 constellations. Pegasus is bordered by Andromeda to the north and east, Lacerta to the north, Cygnus to the northwest, Vulpecula, Delphinus and Equuleus to the west, Aquarius to the south and Pisces to the south and east. The three-letter abbreviation for the constellation, as adopted by the IAU in 1922, is ‘Peg’. The official constellation boundaries, as set by Eugène Delporte in 1930, are defined as a polygon of 35 segments. In the equatorial coordinate system the right ascension coordinates of these borders lie between 21h 12.6m and 00h 14.6m, while the declination coordinates are between 2.33° and 36.61°. Its position in the Northern Celestial Hemisphere means that the whole constellation is visible to observers north of 53°S.[a]
Pegasus is dominated by a roughly square asterism, although one of the stars, Delta Pegasi or Sirrah, is now officially considered to be Alpha Andromedae, part of Andromeda, and is more usually called “Alpheratz”. Traditionally, the body of the horse consists of a quadrilateral formed by the stars α Peg, β Peg, γ Peg, and α And. The front legs of the winged horse are formed by two crooked lines of stars, one leading from η Peg to κ Peg and the other from μ Peg to 1 Pegasi. Another crooked line of stars from α Peg via θ Peg to ε Peg forms the neck and head; ε is the snout.
Bayer catalogued what he counted as 23 stars in the constellation, giving them the Bayer designations Alpha to Psi. He saw Pi Pegasi as one star, and was uncertain of its brightness, wavering between magnitude 4 and 5. Flamsteed labelled this star 29 Pegasi, but Bode concluded that the stars 27 and 29 Pegasi should be Pi1 and Pi2 Pegasi and that Bayer had seen them as a single star. Flamsteed added lower case letters e through to y, omitting A to D as they had been used on Bayer’s chart to designate neighbouring constellations and the equator. He numbered 89 stars (now with Flamsteed designations), though 6 and 11 turned out to be stars in Aquarius. Within the constellation’s borders there are 177 stars of apparent magnitude 6.5 or greater.[b]
Epsilon Pegasi, also known as Enif, marks the horse’s muzzle. The brightest star in Pegasus, is an orange supergiant of spectral type K21b that is around 12 times as massive as the Sun and is around 690 light-yearsdistant from Earth. It is an irregular variable, its apparent magnitude varying between 2.37 and 2.45. Lying near Enif is AG Pegasi, an unusual star that brightened to magnitude 6.0 around 1885 before dimming to magnitude 9. It is composed of a red giant and white dwarf, estimated to be around 2.5 and 0.6 times the mass of the Sun respectively. With its outburst taking over 150 years, it has been described as the slowest novaever recorded.
Three stars with Bayer designations that lie within the Great Square are variable stars. Phi and Psi Pegasi are pulsating red giants, while Tau Pegasi, also known as Kerb, is a Delta Scuti variable—a class of short period (six hours at most) pulsating stars that have been used as standard candles and as subjects to study astroseismology. Rotating rapidly with a projected rotational velocity of 150 km s−1, Kerb is almost 30 times as luminous as the Sun and has a pulsation period of 56.5 minutes. With an outer atmosphere at an effective temperature of 7,762 K,it a white star with a spectral type of A5IV.
Zeta, Xi, Rho and Sigma Pegasi mark the horse’s neck. The brightest of these with a magnitude of 3.4 is Zeta, also traditionally known as Homam. Lying seven degrees southwest of Markab, it is a blue-white main sequence star of spectral type B8V located around 209 light-years distant. It is a slowly pulsating B star that varies slightly in luminosity with a period of 22.952 ± 0.804 hours, completing 1.04566 cycles per day.Xi lies 2 degrees northeast, and is a yellow-white main sequence star of spectral type F6V that is 86% larger and 17% more massive that the Sun, and radiate 4.5 times the solar luminosity. It has a red dwarf companion that is 192.3 au distant. If (as is likely) the smaller star is in orbit around the larger star, then it would take around 2000 years to complete a revolution. Theta Pegasi marks the horse’s eye. Also known as Biham, it is a 3.43-magnitude white main sequence star of spectral type A2V, around 1.8 times as massive, 24 times as luminous, and 2.3 times as wide as the Sun.
Alpha (Markab), Beta (Scheat), and Gamma (Algenib), together with Alpha Andromedae (Alpheratz or Sirrah) form the large asterism known as the Square of Pegasus. The brightest of these, Alpheratz was also known as both Delta Pegasi and Alpha Andromedae before being placed in Andromeda in 1922 with the setting of constellation boundaries. The second brightest star is Scheat, a red giant of spectral type M2.5II-IIIe located around 196 light-years away from Earth. It has expanded until it is some 95 times as large, and has a total luminosity 1,500 times that of the Sun. Beta Pegasi is a semi-regular variable that varies from magnitude 2.31 to 2.74 over a period of 43.3 days. Markab and Algenib are blue-white stars of spectral types B9III and B2IV located 133 and 391 light-years distant respectively. Appearing to have moved off the main sequence as their core hydrogen supply is being or has been exhausted, they are enlarging and cooling to eventually become red giant stars. Markab has an apparent magnitude of 2.48, while Algenib is a Beta Cephei variable that varies between magnitudes 2.82 and 2.86 every 3 hours 38 minutes, and also exhibits some slow pulsations every 1.47 days.
Eta and Omicron Pegasi mark the left knee and Pi Pegasi the left hoof, while Iota and Kappa Pegasi mark the right knee and hoof. Also known as Matar, Eta Pegasi is the fifth-brightest star in the constellation. Shining with an apparent magnitude of 2.94, it is a multiple star system composed of a yellow giant of spectral type G2 and a yellow-white main sequence star of spectral type A5V that are 3.2 and 2.0 times as massive as our Sun. The two revolve around each other every 2.24 years. Farther afield is a binary system of two G-type main sequence stars, that would take 170,000 years to orbit the main pair if they are in fact related. Omicron Pegasi has a magnitude of 4.79. Located 300 ± 20 light-years distant from Earth, it is a white subgiant that has begun to cool, expand and brighten as it exhausts its core hydrogen fuel and moves off the main sequence. Pi1 and Pi2 Pegasi appear as an optical double to the unaided eye as they are separated by 10 arcminutes, and are not a true binary system. Located 289 ± 8 light-years distant, Pi1 is an ageing yellow giant of spectral type G6III, 1.92 times as massive and around 200 times as luminous as the Sun. Pi2 is a yellow-white subgiant that is 2.5 times as massive as the Sun and has expanded to 8 times the Sun’s radius and brightened to 92 times the Sun’s luminosity. It is surrounded by a circumstellar disk spinning at 145 km a second, and is 263 ± 4 light-years distant from Earth.
IK Pegasi is a close binary comprising an A-type main-sequence star and white dwarf in very close orbit; the latter a candidate for a future type Ia supernova as its main star runs out of core hydrogen fuel and expands into a giant and transfers material to the smaller star.
Twelve star systems have been found to have exoplanets. 51 Pegasi was the first Sun-like star discovered to have an exoplanet companion; 51 Pegasi b (unofficially named Bellerophon) is a hot Jupiter close to its sun, completing an orbit every four days. Spectroscopic analysis of HD 209458 b, an extrasolar planet in this constellation, has provided the first evidence of atmospheric water vapor beyond the solar system, while extrasolar planets orbiting the star HR 8799 also in Pegasus are the first to be directly imaged. V391 Pegasi is a hot subdwarf star that has been found to have a planetary companion.
|Markab||α||Arabic||the saddle of the horse|
|Homam||ζ||Arabic||man of high spirit|
|Matar||η||Arabic||lucky rain of shooting stars|
|Sadalbari||μ||Arabic||luck star of the splendid one|
M15 (NGC 7078) is a globular cluster of magnitude 6.4, 34,000 light-years from Earth. It is a Shapley class IV cluster, which means that it is fairly rich and concentrated towards its center. M15 was discovered in 1746 by Jean-Dominique Maraldi.
NGC 7331 is a spiral galaxy located in Pegasus, 38 million light-years distant with a redshift of 0.0027. It was discovered by musician-astronomer William Herschel in 1784 and was later one of the first nebulous objects to be described as “spiral” by William Parsons. Another of Pegasus’s galaxies is NGC 7742, a Type 2 Seyfert galaxy. Located at a distance of 77 million light-years with a redshift of 0.00555, it is an active galaxy with a supermassive black hole at its core. Its characteristic emission lines are produced by gas moving at high speeds around the central black hole.
Pegasus is also noted for its more unusual galaxies and exotic objects. Einstein’s Cross is a quasar that has been lensed by a foreground galaxy. The elliptical galaxy is 400 million light-years away with a redshift of 0.0394, but the quasar is 8 billion light-years away. The lensed quasar resembles a cross because the gravitational force of the foreground galaxy on its light creates four images of the quasar. Stephan’s Quintet is another unique object located in Pegasus. It is a cluster of five galaxies at a distance of 300 million light-years and a redshift of 0.0215. First discovered by Édouard Stephan, a Frenchman, in 1877, the Quintet is unique for its interacting galaxies. Two of the galaxies in the middle of the group have clearly begun to collide, sparking massive bursts of star formation and drawing off long “tails” of stars. Astronomers have predicted that all five galaxies may eventually merge into one large elliptical galaxy.
USS Pegasus (AK-48) and USS Pegasus (PHM-1) are United States navy ships named after the constellation “Pegasus”.
LUNAR FEATURE OF THE MONTH
Mare Humorum Coordinates Coordinates: Diameter 389 km (242 mi) Eponym Sea of Moisture
It was not sampled by the Apollo program, so a precise age has not been determined. However, geological mapping indicates that it is intermediate in age between the Imbrium and Nectaris Basins, suggesting an age of about 3.9 billion years. Humorum Basin is filled with a thick layer of mare basalt, believed to exceed 3 kilometers in thickness at the center of the basin.
A mass concentration (mascon), or gravitational high, was identified in the center of Mare Humorum from Doppler tracking of the five Lunar Orbiter spacecraft in 1968. The mascon was confirmed and mapped at higher resolution with later orbiters such as Lunar Prospector and GRAIL.
On the north edge of Mare Humorum is the large crater Gassendi, which was considered as a possible landing site for Apollo 17. To the south are the floor-fractured Vitello crater, the partially flooded Doppelmayer, and the smaller Puiseux. To the east are Hippalus crater and Promontorium Kelvin. To the west are the Rimae Doppelmayer and the Rupes Liebig, which are cliffs near Liebig itself which is just west of the mare.
Gravity map based on GRAIL
Like most of the other maria on the Moon, Mare Humorum was named by Giovanni Riccioli, whose 1651 nomenclature system has become standardized. Previously, the 17th century astronomer Pierre Gassendi had named it Anticaspia (‘opposite to the Caspian’, referring to Mare Crisium, which he had named after the Caspian Sea), and Michael Van Langren had labelled it the Mare Venetum (“Venetian Sea”) in his 1645 map. Johannes Hevelius called it Sinus Sirbonis (“Bay of Serbonis”, after the lake of Serbonis, now Lake Bardawil, in Egypt) in his 1647 map.
- Wood, Chuck (April 12, 2007). “Ring the Bell II”. Lunar Photo of the Day. Retrieved 2017-01-29.
Gassendi Coordinates Coordinates: Diameter 110 km Depth 1.9 km Colongitude 40° at sunrise Eponym Pierre Gassendi
Gassendi is a large lunar crater feature located at the northern edge of Mare Humorum. The formation has been inundated by lava during the formation of the mare, so only the rim and the multiple central peaks remain above the surface. The outer rim is worn and eroded, although it retains a generally circular form. A smaller crater – Gassendi A – intrudes into the northern rim, and joins a rough uplift at the northwest part of the floor. The crater pair bear a curious resemblance to a diamond ring.
In the southern part of the crater floor is a semi-circular ridge-like formation that is concentric with the outer rim. It is in the southern part where the rim dips down to its lowest portion, and a gap appears at the most southern point. The rim varies in height from as little as 200 meters to as high as 2.5 kilometers above the surface. The floor has numerous hummocks and rough spots. There is also a system of rilles that criss-crosses the floor, named the Rimae Gassendi.
On some older maps the crater Gassendi A was called Clarkson, after the British amateur astronomer and selenographer Roland L. T. Clarkson, but this name is not officially recognized by the IAU and the name has been removed.
By convention these features are identified on lunar maps by placing the letter on the side of the crater midpoint that is closest to Gassendi.
Gassendi Coordinates Diameter, km A 32 B 25 E 7 F 8 G 7 J 9 K 6 L 5 M 3 N 4 O 10 P 2 R 4 T 10 W 6 Y 5