Orion Arm


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For the stars which form the arm of the Orion asterism, see Orion (constellation). For the online project, see Orion's Arm.
New view of the Milky Way with four clearly defined and symmetric spiral arms[1]
Observed structure of the Milky Way's spiral arms[2]

The Orion Arm is a minor spiral arm of the Milky Way Galaxy that is 3,500 light-years (1,100 parsecs) across and approximately 10,000 light-years (3,100 parsecs) in length,[3] containing the Solar System, including Earth. It is also referred to by its full name, the Orion–Cygnus Arm, as well as Local Arm, Orion Bridge, and formerly, the Local Spur and Orion Spur.

Milky Way centre from Sinai, Egypt

The arm is named for the Orion Constellation, which is one of the most prominent constellations of Northern Hemisphere winter (Southern Hemisphere summer). Some of the brightest stars and most famous celestial objects of the constellation (e.g. Betelgeuse, Rigel, the three stars of Orion's Belt, the Orion Nebula) are within it as shown on the interactive map below.

The arm is between the Carina–Sagittarius Arm (the local portions of which are toward the Galactic Center) and the Perseus Arm (the local portion of which is the main outer-most arm and one of two major arms of the galaxy).

Long thought to be a minor structure, namely a "spur" between the two arms mentioned, evidence was presented in mid 2013 that the Orion Arm might be a branch of the Perseus Arm, or possibly an independent arm segment.[4]

Within the arm, the Solar System is close to its inner rim, in a relative cavity in the arm's Interstellar Medium known as the Local Bubble, about halfway along the arm's length, approximately 8,000 parsecs (26,000 light-years) from the Galactic Center.

Recently, more than 30 methanol (6.7-GHz) and water (22-GHz) masers in high-mass star-forming regions around sun have been measured their parallax and proper motions with the distance accuracy of better than ±10% and even 3%, the best parallax measurement in the BeSSeL project. The accuracy locations of interstellar masers in HMSFRs have been shown that the Local arm appears to be an orphan segment of an arm between the Sagittarius and Perseus arms that wraps around less than a quarter of the Milky Way. The segment has the length of ~20,000 ly and the width of ~3,000 ly with the pitch angle from 10.1° ± 2.7° to 11.6° ± 1.8°. These results reveal that the Local Arm is larger than previously thought, and both its pitch angle and star formation rate are comparable to those of the Galaxy’s major spiral arms. The Local arm is reasonably referred the fifth feature in the Milky Way. The “spur” interpretation may be incorrect.[1][5][6][7][8]

To understand the form of the Local arm between the Sagittarius and Perseus arms, the stellar density of a specific population of stars with about 1 Gyr of age between 90° ≤ l ≤ 270° have been mapped using the Gaia DR2.[9] The 1 Gyr population have been employed because they are significantly evolved objects than the gas in HMSFRs tracing Local arm. An interesting investigations have been carried out to compare both the stellar density and gas distribution along Local arm. Researchers have found a marginally significant arm-like stellar overdensity close to the Local Arm, identified with the HMSFRs especially in the region of 90° ≤ l ≤ 190°.[10] They have concluded the Local Arm as the arm segment associated with only the gas and star-forming clouds, but a significant stellar overdensity. Additionally they have found that the pitch angle of the stellar arm is slightly larger than the gas-defined arm, and also there is an offset between gas-defined and stellar arm. The offset and different pitch angles between the stellar and HMSFR-defined spiral arms are consistent with the expectation that star formation lags the gas compression in a spiral density wave lasting longer than the typical star formation timescale of 107 − 108 years.[11]

Messier objects

The shape of the Orion Spur[12]

The Orion Arm contains a number of Messier objects:

Interactive maps

Rosette NebulaOrion NebulaTrifid NebulaLagoon NebulaOmega NebulaEagle NebulaNorth America NebulaRigelPolarisSunBetelgeuseDenebPerseus ArmOrion ArmSagittarius Arm
Orion and neighboring arms (clickable map)
Rosette NebulaCone NebulaCalifornia NebulaHeart NebulaOrion NebulaSoul NebulaNorth America NebulaVeil NebulaTrifid NebulaCrescent NebulaLagoon NebulaOmega NebulaEagle NebulaEta Carinae NebulaMessier 37Messier 36Messier 38Messier 50Messier 46Messier 67Messier 34Messier 48Messier 41Messier 47Messier 39Messier 52Messier 93Messier 7Messier 25Messier 23Messier 21Messier 18Messier 26Messier 35NGC 2362NGC 3532IC 2602NGC 6087NGC 3766IC 4665IC 2944NGC 6231Messier 103Messier 29Perseus ArmOrion ArmSagittarius ArmNebula
The nearest nebulae and star clusters (clickable map)

See also

References

  1. ^ a b Reid, Mark; Zheng, Xing-Wu (2020). A New Map of the Milky Way. April. Scientific American.
  2. ^ See the "Spiral Arms" part of this NASA animation for details
  3. ^ Harold Spencer Jones, T. H. Huxley, Proceedings of the Royal Institution of Great Britain, Royal Institution of Great Britain, v. 38–39
  4. ^ Earth's Milky Way Neighborhood Gets More Respect, National Radio Astronomy Observatory, Dave Finley, 3 June 2013
  5. ^ Xu, Y., Reid, M., Xu, Y., Reid, M., Dame, T., et al. 2016, SciA, 2, e1600878
  6. ^ Xu ,Y., Li, J. J., Reid,Xu ,Y., Li, J. J., Reid, M. J., et al. 2013,.ApJ, 769, 15.
  7. ^ Reid, M. J., Menten,Reid, M. J., Menten, K. M., Brunthaler, A., et al. 2019, ApJ, 885,18
  8. ^ Hirota,T., Nagayama,T., Hirota,T., Nagayama,T., Honma,M., et al. 2020, PASJ,72,50
  9. ^ Miyachi1, Y.,Miyachi1, Y., Sakai, N., Kawata, D., et al.2019,ApJ, 882,48
  10. ^ Hirota, T., Hirota, T., Nagayama, T., Honma, M., et al. 2020, PASJ,72,50
  11. ^ Shen, j., and Zheng, X.,Shen, j., and Zheng, X., 2020, RAA, Vol.20, No.10,159
  12. ^ Vázquez, Ruben A.; May, Jorge; Carraro, Giovanni; Bronfman, Leonardo; Moitinho, André; Baume, Gustavo (January 2008). "Spiral Structure in the Outer Galactic Disk. I. The Third Galactic Quadrant". The Astrophysical Journal. 672 (2): 930–939. arXiv:0709.3973. Bibcode:2008ApJ...672..930V. doi:10.1086/524003.

External links

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