Julian Date: 2459037.16
2019-2020: CLXXI
THE DAILY ASTRONOMER
Monday, July 6, 2020
Remote Planetarium 59: Intrinsic Variables II - Long Period Variables
Let's begin the week by discussing a star called "wonderful." Known by the actual name "Mira," this star marks the long throat connecting the faint head and larger body of Cetus, the seamonster. One can observe Cetus in the early morning eastern sky this time of year. While seeing Cetus, an observer might or might not find Mira because for much of the year it won't be visible to the unaided eye. Its brightness varies from a magnitude of 10.1 (minimum) to a magnitude of 2.0 (maximum.) When a star's magnitude is 6.0 or higher, it generally isn't visible to the unaided eye.
Mira is the archetype of the "Mira Variables," defined as those stars that are passing through the latter stages of their life cycles. Their masses are generally less than two solar masses. Mira variables are fusing helium in their cores and will soon expel their outer layers as planetary nebulae before leaving white dwarf remnants behind. Unlike Cepheid variables that pulsate in response to helium ionization in specific layers, Mira variables pulsate because the entire star is expanding and contracting due to turbulent changes within the inner layers. This turbulence relates in part to the motions of the hydrogen-burning shell enveloping the helium burning core. Another difference relates to the substantial brightness changes. Whereas a Cepheid variable's brightness diminishes and increases as the size and temperature increase and decrease, the brightness of a Mira variable will change as energy shifts from the visual to the infra-red part of the electromagnetic spectrum. As Mira variables are solar mass stars toward the end of their lives, they will actually be red giants: much larger than the Sun, but also significantly cooler. Also, recent observations have revealed that Mira variables tend to be enshrouded in diffuse shells containing carbon dioxide, water vapor and other molecules that will affect the star's apparent brightness.
Mira variables are distinguished by the following characteristics:
- periods between 80 - 1000 days
- masses comparable to that of the Sun.
- toward the end of their life cycles (Red Giant stage)
- the range of brightness variations can extend many magnitudes
Mira's variability period is 332 days. So, one can expect it to reach its maximum brightness once a year. The following list includes the upcoming dates of Mira maxima. Fortunately, the next Mira maximum occurs around mid to late September, the time of year when its host constellation Cetus is well placed for evening viewing.
Mira Maxima:
- September 20, 2020
- August 18, 2021
- July 16, 2022
- June 13, 2023
The "Mira Light Curve." We see the variations in Mira's brightness over time in the above light curve. Notice that the minima and maxima are not consistent, but instead can vary by as much as a magnitude.
___________________________________________________
Rapid astronomer profile: Johannes Hevelius (1611-1687). Yes, we've encountered him before. We saw Hevelius when we were discussing constellations of relatively recent coinage. (He crafted a few of them, himself.) Hevelius named the star "Mira," meaning "wonderful," because of its tendency to appear and then reappear. He first included the name in his 1662 publication "Historiola Mirae Stellae ," (A Short History of the Wonderful Star.)
_____________________________________________
When at maximum brightness (magnitude 2.0) Mira is the brightest of the Mira variables. The next brightest of Chi Cygni, a star within Cygnus the Swan:
Chi Cygni is marked by the black dot to the right of the vertical axis of the "Northern Cross" which is just under Eta Cygni. Chi Cygni's mean variability period lasts 408 days. At brightest, Chi Cygni's magnitude equals 3.3. At its dimmest, the magnitude is approximately 14.1, almost 1600 times dimmer than the faintest naked eye stars. Because the variability period can itself vary by as much as forty days, we will not post the same maxima calendar we produced for Mira. Besides, Chi Cygni at maximum is three times dimmer than Mira at maximum.
The Mira-type is the main type of long period variable star. The only other type is the "semi regular variable," those whose variability itself varies considerably due to interior turbulence. Astronomers divide semi-regular (SR) variables into four categories (a - d).
Perhaps the most famous example of a semi-regular variable is Betelgeuse, the star marking Orion's eastern shoulder. (Orion isn't currently visible due to its close proximity to the Sun.) Betelgeuse is also toward the end of its life cycle and exhibits irregular variability due to a variety of complex factors, including alterations in its magnetic field and the conveyance of energy through its dynamic outer layers. In fact, just within the last year we observed Betelgeuse's brightness diminish considerably. Many of us wondered if that red supergiant star was about to explode as a Type II supernova. It turned out that the dimming was merely part of the irregular variability cycle and not a precursor to an imminent explosion.
All long period variables, be they Mira-type or semi-regular, are stars nearing the conclusion of their life cycles. It seems likely that most stars will become variable at some point in these cycles: the type of which depends, of course, on the star's mass. After all, a star's entire life cycle depends on its mass.
Tomorrow, part three of our Intrinsic Variable lesson with Cataclysmic Stars.
__________________________________
Skywatching tip: Moon and Saturn
Look for the moon near Saturn this evening! The moon still will appear full tonight. The moderately bright "star" near the moon is Saturn, the most distant planet visible to the unaided eye.
____________________________________
To subscribe or unsubscribe from the Daily Astronomer: