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From Wikipedia, the free encyclopedia

TU Muscae

A light curve for TU Muscae, plotted from TESS data[1]
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Musca
Right ascension 11h 31m 10.92470s[2]
Declination −65° 44′ 32.1019″[2]
Apparent magnitude (V) 8.307[3](8.17 - 8.75[4])
Characteristics
Spectral type O7V + O8V[5]
U−B color index −0.860[3]
B−V color index +0.047[3]
Variable type β Lyr[4]
Astrometry
Radial velocity (Rv)−4[6] km/s
Proper motion (μ) RA: −6.62[2] mas/yr
Dec.: −1.21[2] mas/yr
Parallax (π)0.02 ± 0.76 mas[2]
Orbit[5]
Period (P)1.387 days
Semi-major axis (a)17.34 R[7]
Eccentricity (e)0
Inclination (i)77.7°
Longitude of the node (Ω)3.137[6]°
Semi-amplitude (K1)
(primary)
214.5 km/s
Semi-amplitude (K2)
(secondary)
345.8 km/s
Details[5]
Primary
Mass16.8 M
Radius7.2 R
Luminosity105,000 L
Surface gravity (log g)4.05[7] cgs
Temperature35,000[6] K
secondary
Mass10.5 M
Radius5.7 R
Luminosity35,000 L
Surface gravity (log g)4.04[7] cgs
Temperature31,366[6] K
Other designations
TU Muscae, HIP 56196, HD 100213, BD−65°1101, 2MASS J11311091-6544322
Database references
SIMBADdata

TU Muscae, also known as HD100213, is an eclipsing binary star in the constellation Musca. Its apparent magnitude ranges from 8.17 to 8.75 over around 1.4 days.[4]

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Transcription

Have you ever noticed something swimming in your field of vision? It may look like a tiny worm or a transparent blob, and whenever you try to get a closer look, it disappears, only to reappear as soon as you shift your glance. But don't go rinsing out your eyes! What you are seeing is a common phenomenon known as a floater. The scientific name for these objects is Muscae volitantes, Latin for "flying flies," and true to their name, they can be somewhat annoying. But they're not actually bugs or any kind of external objects at all. Rather, they exist inside your eyeball. Floaters may seem to be alive, since they move and change shape, but they are not alive. Floaters are tiny objects that cast shadows on the retina, the light-sensitive tissue at the back of your eye. They might be bits of tissue, red blood cells, or clumps of protein. And because they're suspended within the vitreous humor, the gel-like liquid that fills the inside of your eye, floaters drift along with your eye movements, and seem to bounce a little when your eye stops. Floaters may be only barely distinguishable most of the time. They become more visible the closer they are to the retina, just as holding your hand closer to a table with an overhead light will result in a more sharply defined shadow. And floaters are particularly noticeable when you are looking at a uniform bright surface, like a blank computer screen, snow, or a clear sky, where the consistency of the background makes them easier to distinguish. The brighter the light is, the more your pupil contracts. This has an effect similar to replacing a large diffuse light fixture with a single overhead light bulb, which also makes the shadow appear clearer. There is another visual phenomenon that looks similar to floaters but is in fact unrelated. If you've seen tiny dots of light darting about when looking at a bright blue sky, you've experienced what is known as the blue field entoptic phenomenon. In some ways, this is the opposite of seeing floaters. Here, you are not seeing shadows but little moving windows letting light through to your retina. The windows are actually caused by white blood cells moving through the capillaries along your retina's surface. These leukocytes can be so large that they nearly fill a capillary causing a plasma space to open up in front of them. Because the space in the white blood cells are both more transparent to blue light than the red blood cells normally present in capillaries, we see a moving dot of light wherever this happens, following the paths of your capillaries and moving in time with your pulse. Under ideal viewing conditions, you might even see what looks like a dark tail following the dot. This is the red blood cells that have bunched up behind the leukocyte. Some science museums have an exhibit which consists of a screen of blue light, allowing you to see these blue sky sprites much more clearly than you normally would. While everybody's eyes experience these sort of effects, the number and type vary greatly. In the case of floaters, they often go unnoticed as our brain learns to ignore them. However, abnormally numerous or large floaters that interfere with vision may be sign of a more serious condition, requiring immediate medical treatment. But the majority of the time entoptic phenomena, such as floaters and blue sky sprites, are just a gentle reminder that what we think we see depends just as much on our biology and minds as it does on the external world.

Physical description

TU Muscae is a remote binary star system made up of two hot luminous blue main sequence stars of spectral types O7.5V and O9.5V, with masses 23 and 15 times that of the Sun. The stars are so close that they are in contact with each other (overcontact binary) and are classed as a Beta Lyrae variable as their light varies from earth as they eclipse each other.[6] The spectra indicate they are hot stars, with surface temperatures of roughly 37200 and 34700 K respectively. They are both still on the main sequence of star evolution, burning their core hydrogen. Astronomers Laura Penny and Cynthia Ouszt proposed the two were originally more equal in size but as they became close enough so that material from the less massive star began transferring to the more massive star via Roche-lobe overflow. However they concede that figuring out the evolution of interacting massive binary systems is "a little like trying to unspill milk".[5] The system is thought to be around 4.8 kiloparsecs (~15500 light-years) distant.[6]

The period of the magnitude change is increasing, and has been calculated as lengthening by 3.46 seconds a century. This could be due to material from the less massive star being transferred to the more massive one, or there could be a third or fourth as yet undetected star in the multiple star system influencing the orbit. These stars have not been seen as they are much less luminous than the two main stars.[8]

Discovery

TU Muscae was discovered by Dutch astronomer Pieter Oosterhoff in 1928. Initially thought to have a spectrum of B3, later observations in the 1960s and early 1970s indicated it was a hotter star than previously thought—with the spectrum lying in the uncommon O-region.[9]

References

  1. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. ^ a b c d e Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.
  3. ^ a b c Maíz-Apellániz, Jesús; Walborn, Nolan R.; Galué, Héctor Á.; Wei, Lisa H. (2004). "A Galactic O Star Catalog". The Astrophysical Journal Supplement Series. 151 (1): 103–148. arXiv:astro-ph/0311196. Bibcode:2004ApJS..151..103M. doi:10.1086/381380. S2CID 118813863.
  4. ^ a b c Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  5. ^ a b c d Penny, Laura R.; Ouzts, Cynthia (2009). "Tomographic Separation of Composite Spectra. XI. The Physical Properties of the Massive Close Binary HD 100213 (TU Muscae)". The Astrophysical Journal. 681 (1): 554–61. arXiv:0905.3687. Bibcode:2008ApJ...681..554P. doi:10.1086/587509. S2CID 16333964.
  6. ^ a b c d e f Terrell, Dirk; Munari, Ulisse; Zwitter , Tomaˇz; Nelson, Robert H. (2003). "Observational Studies of Early-type Overcontact Binaries: TU Muscae". The Astronomical Journal. 126 (6): 2988–96. arXiv:astro-ph/0309366. Bibcode:2003AJ....126.2988T. doi:10.1086/379678. S2CID 6445980.
  7. ^ a b c Palate, M.; Rauw, G. (2012). "Spectral modelling of circular massive binary systems. Towards an understanding of the Struve-Sahade effect?". Astronomy & Astrophysics. 537: A119. arXiv:1109.1103. Bibcode:2012A&A...537A.119P. doi:10.1051/0004-6361/201117520. S2CID 84840295.
  8. ^ Qian, S.-B.; Yuan, J.-Z.; Liu, L.; He, J.-J.; Fernández Lajús, E.; et al. (2007). "Evolutionary states of the two shortest period O-type overcontact binaries V382 Cyg and TU Mus". Monthly Notices of the Royal Astronomical Society. 380 (4): 1599–1607. Bibcode:2007MNRAS.380.1599Q. doi:10.1111/j.1365-2966.2007.12184.x. hdl:11336/41984. S2CID 121158760.
  9. ^ Andersen, J.; Grønbech, B. (1975). "The close 0-type eclipsing binary TU Muscae". Astronomy & Astrophysics. 45: 107–15. Bibcode:1975A&A....45..107A.
This page was last edited on 14 May 2023, at 12:24
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