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1-Methylnaphthalene

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1-Methylnaphthalene[1]
Names
IUPAC name
1-Methylnaphthalene
Other names
α-methylnaphthalene
Identifiers
3D model (JSmol)
ChEBI
ChEMBL
ChemSpider
ECHA InfoCard 100.001.788 Edit this at Wikidata
EC Number
  • 201-966-8
KEGG
  • InChI=1S/C11H10/c1-9-5-4-7-10-6-2-3-8-11(9)10/h2-8H,1H3 checkY
    Key: QPUYECUOLPXSFR-UHFFFAOYSA-N checkY
  • InChI=1/C11H10/c1-9-5-4-7-10-6-2-3-8-11(9)10/h2-8H,1H3
    Key: QPUYECUOLPXSFR-UHFFFAOYAD
  • c1cccc2cccc(c12)C
Properties
C11H10
Molar mass 142.20 g/mol
Appearance Liquid
Density 1.001 g/mL
Melting point −22 °C (−8 °F; 251 K)
Boiling point 240–243 °C (464–469 °F; 513–516 K)
Vapor pressure 4.91
Hazards
Flash point 82 °C (180 °F; 355 K)
Except where otherwise noted, data are given for materials in their standard state (at 25 °C [77 °F], 100 kPa).
checkY verify (what is checkY☒N ?)

1-Methylnaphthalene is a polycyclic aromatic hydrocarbon (PAH). It has a cetane number of zero, and was previously used as the lower reference for cetane number. However, due to the expense and handling difficulty of 1-methylnaphthalene, it was replaced in this capacity by isocetane, with a CN of 15.[2]

On February 22, 2014, NASA announced a greatly upgraded database[3][4] for detecting and monitoring PAHs, including 1-methylnaphthalene, in the universe. According to NASA scientists, over 20% of the carbon in the universe may be associated with PAHs, possible starting materials for the formation of life.[3] PAHs seem to have been formed shortly after the Big Bang, are abundant in the universe,[5][6][7] and are associated with new stars and exoplanets.[3]

See also

References

  1. ^ 1-Methylnaphthalene at University of Oxford
  2. ^ Cetane number
  3. ^ a b c Hoover, Rachel (February 21, 2014). "Need to Track Organic Nano-Particles Across the Universe? NASA's Got an App for That". NASA. Retrieved February 22, 2014.
  4. ^ Staff (October 29, 2013). "PAH IR Spectral Database". NASA. Retrieved March 12, 2014.
  5. ^ Carey, Bjorn (October 18, 2005). "Life's Building Blocks 'Abundant in Space'". Space.com. Retrieved March 3, 2014.
  6. ^ Hudgins, Douglas M.; Bauschlicher Jr, Charles W.; Allamandola, L. J. (October 10, 2005). "Variations in the Peak Position of the 6.2 μm Interstellar Emission Feature: A Tracer of N in the Interstellar Polycyclic Aromatic Hydrocarbon Population". Astrophysical Journal. 632: 316–332. doi:10.1086/432495. Retrieved March 3, 2014.
  7. ^ Allamandola, Louis; et al. (April 13, 2011). "Cosmic Distribution of Chemical Complexity". NASA. Retrieved March 3, 2014.


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