Our NOVA Newsletter for Sep-Oct 2020 is available as a pdf file. An archive of older issues can be found on our Newsletter page. The contents include:

At Last, a Naked-Eye Comet by J. Karl Miller

President’s Message by Gordon Farrell

The Five Ws for Mars at Opposition by Ken Jackson

2020 Martha Ellen Pearse Award by Suzanna Nagy

The upcoming opposition of Mars promises to be an exciting event for planetary observers – here is the Who, What, When, Where, and Why on the 2020 opposition.

Who: The planet Mars and you – to observe it! Mars is the 4th planet from the Sun and is named after the Roman god of war. It is also called the red planet because of its rusty red surface. It is the second smallest planet with a diameter that is about ½ that of Earth’s and whose gravity is only 37.5% of Earth’s. A big attraction of Mars as an observing target is that it is the only planet to reveal its surface features to us with backyard telescopes with oppositions being the best times for a chance to view those features.

What: Oppositions occur when the Earth passes directly between an outer planet and the Sun placing the planet opposite the Sun in our sky – the planet rises when the Sun sets and it can be viewed throughout the entire night. An added bonus is that a planet at opposition is close to Earth and therefore appears bigger and brighter.

Mars displays the greatest changes in size because it is the first outer planet away from the Sun from us. It can go from being a fairly small and faint dot to the 2nd brightest planet in the sky (after Venus). Surface features like the polar ice caps, volcanoes, and darker regions of exposed volcanic rock become visible at opposition. A Martian sol lasts slightly longer than an Earth day so new surface features appear night after night and you get a chance to see much of Mars’ surface in the weeks surrounding opposition. Mars appears small, even at its maximum size, so a telescope is required to see surface features. Bumping up the magnification and some patience can help in picking out the details.

When: Opposition occurs at 23:20 UT on October 13, 2020. That is 04:20 pm Pacific Daylight Time but you don’t need to aim for the exact date or time – views of Mars will be good for several weeks around opposition. In fact, Mars makes its closest approach to Earth on Oct 6, 2020, a little bit earlier than the opposition date due to the elliptical (non-circular) shape of its orbit.

Oppositions of Mars occur on average every 780 days or approximately every 26 months. The distance from Earth to Mars varies between oppositions as does its size. Mars will be about 0.41 AU from Earth at this year’s 2020 opposition with a size of 22.6 arc-seconds. The 2020 opposition ranks high with respect to distance and size as Mars will not be as close nor as big during the next three oppositions in 2022, 2025, and 2027.

Where: Mars will be in a good position for observers in the Northern Hemisphere during its 2020 opposition. Mars will rise in the east at sundown (06:30 pm PDT) and will climb higher into south-eastern and southern skies closer to midnight. It reaches a maximum altitude at opposition of 46 degrees above the horizon at 1:00 am PDT on Oct 14th – there is likely to be better seeing and less atmospheric distortion with Mars that high in the sky.

Why: Oppositions of Mars occur because the orbits of Mars and the Earth make them align in a straight line with the Sun where the Sun and Mars are on opposite sides of the Earth.

The Earth moves more quickly in its orbit than Mars so it passes and then catches back up to Mars every 780 days on average.

That’s it. Go out and see Mars for yourself. Try to observe it over a few nights around the opposition to take in more of its surface. Keep an eye on this website for additional upcoming articles on Mars. With some luck with the weather and clear skies, Mars will reveal its surface details to us Earthbound observers.

A few years ago I wanted to have a look at the Triangulum Galaxy M33 from my yard in Coquitlam. There’s a significant amount of light pollution – I’d estimate the sky to be Bortle class 7 to 8. Despite that, I am able to see bright Messier objects like the Globular Cluster M13, the Ring Nebula M57, and the Bode’s Galaxy M81. M33 was more challenging. I tried several different nights but had no success in spotting it. Confused and frustrated, I checked the magnitude in Stellarium as I knew magnitude is a measure of an object’s brightness. Stellarium showed M33’s magnitude as 5.7 – quite bright and definitely brighter than the other objects I could see: M13 at 5.8, M57 at 8.8, and M81 at 6.94 (remember that brighter objects have a lower magnitude). So why couldn’t I pick out M33?

I have since learned that magnitude works well for stars but it is not a good indicator of how easy or hard it is to see deep sky objects that cover an extended area – aka extended objects. Magnitude assumes all the light is concentrated in a single point source like a star but M33 covers an area of approximately 65 x 40 arc minutes and its light is spread over this entire area.

A better measure is “surface brightness”: the average brightness over the extended area. Surface brightness is often measured in magnitudes per square arcsecond. M33 has a surface brightness of 23 mag/arcsec^2. If you divide the area of M33 into a bunch of little 1 arcsecond squares then on average each square will be as bright as a 23rd magnitude star. As with magnitudes, a lower surface brightness indicates a brighter object. An object with a surface brightness greater than 22 is generally considered to be faint.

Surface brightness is also a good way to measure sky-glow and light pollution. An urban/city sky might have a surface brightness of 17 mag/arcsec^2 while a pristine dark sky might have a surface brightness of 22 mag/arcsec^2. The Canadian company Unihedron makes relatively inexpensive Sky Quality Meters (SQM) used by many amateur astronomers to measure sky-glow. I used Unihedron’s SQM-L and measured the sky-glow at my Coquitlam location to be 18.5 mag/arcsec^2 on a moonless night.

An object can be difficult to detect when its surface brightness is close to or fainter than the sky-glow. Tony Flanders reports barely seeing objects down to a surface brightness of 21 in his skies where the sky-glow is 18 mag/arcsec^2 and he speculates that an object is not detectable if it is more than 3 magnitudes fainter than the sky-glow. With this in mind, it is not surprising that M33 is hard to detect from my Coquitlam location as the surface brightness of M33 is almost 4.5 magnitudes fainter than the sky-glow.

There are other factors involved in whether or not an object is visible. The RASC Oberver’s Handbook section “Magnification and Contrast in Deep-sky Objects” has a good explanation of some of these including the following.

• Surface brightness is not uniform. For example spiral galaxies often have a bright core area that is brighter and easier to see than the arms. Flanders and others suggests that peak surface brightness is an even better indicator of whether or not an extended object is difficult to observe.
• Larger objects are easier to detect so increasing the magnification on faint objects can help.
• Objects like nebula are easier to see when using band filters that increase contrast by darkening the sky-glow more than they darken the light from the nebula.
• Surface brightness may not be a good measure for objects like globular and open clusters that resolve into individual stars.
• The surface brightness of an object is subjective as it depends on the size of the object. How far do the faint arms of a spiral galaxy really extend? 

Several tools can help you find the surface brightness for observing targets:

•  The surface brightness of an object can be displayed in Stellarium if the “Additional information” option in the “Configuration” window is enabled.
• The “Magnitude and Contrast Calculator” is a spreadsheet, included as a supplement to the RASC Observer’s handbook, that calculates the surface brightness and predicts whether an object is visible from telescope, filter, and sky parameters.
• Tony Flanders has compiled a list of Messier objects that includes the surface brightness and peak surface brightness (for some Messier objects). The table below is an excerpt from his list.

Object	Type	Const	Mag	Peak	Surface Bright- ness	Size
M57	Planetary Nebula	Lyr	8.8	17.8	17.8	1.4×1.0
M45	Open Cluster	Tau	1.2	–	19.8	100
M27	Planetary Nebula	Vul	7.3	18.4	20.1	8.0×5.7
M76	Planetary Nebula	Per	10.1	18.6	20.4	2.7×1.8
M24	Star Cloud	Sgr	3.1	–	20.5	95×35
M42	Nebula	Ori	4	–	20.5	40×35
M1	Supernova Remnant	Tau	8.4	–	20.5	6×4
M13	Globular Cluster	Her	5.8	16.9	20.6	17
M31	Galaxy	And	3.4	16.6	22.2	191×62
M33	Galaxy	Tri	5.7	20.1	23	71×42

Comet Neowise is receding from us but the Earth is about to plow through the debris field left behind by the comet 109P/Swift-Tuttle. We’ll see this as the Perseid Meteor shower where dust to pea-size bits of comet material impact the atmosphere and burn up in a trail of glowing ionized gas.

This annual meteor shower occurs over several days, every year, in mid-August. This year, the peak rate is predicted to occur on the night of Tuesday, August 11th at 11:00 pm PDT but Perseid meteors will be active for several days surrounding the peak.

Comet Swift-Tuttle is a periodic comet that makes a return trip close to the Sun and Earth every 133 years. It comes a little inside Earth’s orbit at its perihelion before heading back out past Pluto. It has a long history of observations with probable sightings as early as 322 BC and 69 BC. In 188, Chinese records suggest it reached naked-eye 0.1  magnitude. Its last close approach was in 1992 when it was visible with binoculars. The next return trip is not until 2126 when it could again be a bright naked-eye comet at 0.7 magnitude.

Perseid meteors can appear anywhere in the sky but they all seem to originate from a fixed point, called the radiant,  near the star Eta Persei in the constellation Perseus – the Hero.  From a dark site, you may be able to see as many as 110 meteors per hour. Note that the Moon rises just after midnight, at 12:05 AM, on August 12th and the moonlight will wash out faint meteors during early morning observing. No special equipment is needed to see the meteors – just lie back in a lawn chair or on the ground and look up and perhaps count how many you see.

The MacMillan Space Centre is hosting a Perseid Meteor Shower celebration on Wednesday, August 12th. The in-person star party is sold-out but you can still register to watch a live stream (by donation) – visit the Space Centre’s event info page to register and for more information.

Scott talks about comet neowise in a July segment of Space Talk with Scott on Global TV – https://globalnews.ca/video/rd/1b6a3b6c-c927-11ea-b200-0242ac110004/?jwsource=cl

See our post on How to Find Comet Neowise for a chart and other tips.

Three missions to Mars are getting ready to launch in the next few weeks. Why are all these missions launching at the same time?

They are all timed to match the upcoming Mars opposition on October 13th, 2020. When Mars is at opposition, Mars and the Sun are on opposite sides of the Earth. At opposition, Mars is also at its closest point to the Earth, making it more fuel-efficient for a spacecraft to reach the red planet.

Missions to Mars are often designed to follow a Hohmann transfer orbit to move a spacecraft from a lower circular orbit to a higher circular orbit using the least amount of fuel. A Hohmann transfer orbit involves an initial burn to push the spacecraft into an elliptical orbit, coasting most of the way to the higher orbit, then a second burn to put it into a circular orbit. To meet up with Mars, the transfer orbit also needs to be timed so that the spacecraft reaches the higher orbit at the same time that Mars is there – this timing requirement leads to launch windows that occur a few months before each opposition of Mars. The Mars Insight spacecraft (https://mars.nasa.gov/insight/) launched in May 2018, with the trajectory below, was timed to match up with Mars’ last opposition in July 2018.

Oppositions of Mars occur approximately 26 months apart so missing a launch window means a delay of over two years.

United Arab Emirates – Emirates Mars Mission

Launch Window: July 14 to Aug 12

This science mission from the United Arab Emirates (UAE) — the first by an Arab-Islamic country — will blast-off from Tanegashima Space Center, Japan. The “Hope Probe” seeks to provide a better understanding of the Martian atmosphere and its layers, including the loss of hydrogen and oxygen gases into space over a Martian year.

China National Space Administration (CNSA)’s – Tianwen-1

Launch window: July 23 to Aug 15

The Tianwen-1 mission (known as Huoxing-1, HX-1 during development) will be China’s first Mars orbiter, lander and rover. It will deploy an orbiter around Mars and land a rover on the surface on April 23, 2021. Its stated objectives are to search for evidence of both current and past life and to assess the planet’s environment.

NASA Mars 2020

Launch Window: July 30 to Aug 15

The Mars 2020 mission addresses key astrobiology questions about the potential for life on Mars. The Perseverance rover includes a drill that can collect core samples of the most promising rocks and soils and set them aside in a “cache” on the surface of Mars – ready to be returned to Earth in a future mission.

Delayed: European Space Agency – ExoMars

A fourth mission, the ESA’s ExoMars mission, was originally scheduled to launch in 2020. However, the COVID-19 pandemic impacted the timelines for testing vital parachutes & electronics and forced a delay. But since oppositions of Mars happen every 26 months, the launch has been postponed by over two years to 2022.

The once-in-a-decade Comet Neowise is a spectacular sight in the evening skies from Vancouver.

Here are a few tips for finding the comet.

• Check that the skies are at least partly clear – Vancouver’s Clear Sky Clock: provides a forecast of the cloud cover.
• Try to find a dark site, away from city lights if possible, with a clear view to the north-west.
• Look to the north-west, above the north-shore mountains.
• The comet is visible a little after sundown starting around 10:00 pm.
• It is low on the horizon – at approximately 15° or the width of your hand held out at arms length.
• It is below the Big Dipper. Use the two bottom stars in the bucket of the Big Dipper as a pointer to the end of the tail.
• The comet appears as a faint fuzzy streak to the naked eye.
• The view is spectacular in binoculars. The tail is at least 5 degrees long so it fills most binocular’s field of view.
• The comet moves down closer to the horizon as the it gets later at night.

The comet should be a nice sight for the next few weeks and there are some clear evening skies in the forecast so take the opportunity to have a look. Gary Boyle wrote an article in the Georgia Strait with more information & tips. The article includes the image below showing the progress of the comet during July.

The comet is a great target for photography so bring your camera and get some advice on taking your own photos in the article “A Beginner’s Guide To Photographing Comet Neowise “. Vancouver is Awesome has a great collection of photos from around Vancouver.

The comet will dim in absolute brightness as the month progresses because it is moving further away from the Sun. But it is moving higher in the sky and makes its closest approach on July 23rd so the views and contrast might still improve for another week.

Our NOVA Newsletter for July-Aug 2020 is available as a pdf file. An archive of older issues can be found on our Newsletter page. The contents include:

Barry Shanko 1960-2020 by Chris Gainor

Is the Sun Getting More Active? by J. Karl Miller

President’s Message by Gordon Farrell

The RASC Virtual GA and GA Lite 2020 by RASC Vancouver GA Committee

Memories of Barry by Scott McGillivray

By Milan B

The (Northern) Summer Solstice, today at 2:44 PM PDT, marks the earliest beginning of summer since 1896.

The chart above shows how the quadrennial correction (which the Julian Calendar is solely based on) works well short term, but over a longer period of time (130 years or so), it produces a significant error (one full day). To correct this, the Gregorian Calendar introduces another correction which is to omit leap days in some of the years that centuries begin with (or end, some would say). Years like 1700, 1800, 1900, 2100, 2200, 2300 etc. are chosen for this correction. So, we are in a deep stretch without this centennial correction and the seasons’ start dates will be falling even earlier until late 21st century.