Isotopes of titanium

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Isotopes of titanium  (22Ti)
Main isotopes [1] Decay
abun­dance half-life (t1/2) mode pro­duct
44Ti synth 59.1 y ε 44Sc
46Ti8.25% stable
47Ti7.44%stable
48Ti73.7%stable
49Ti5.41%stable
50Ti5.18%stable
Standard atomic weight Ar°(Ti)

Naturally occurring titanium (22Ti) is composed of five stable isotopes; 46Ti, 47Ti, 48Ti, 49Ti and 50Ti with 48Ti being the most abundant (73.8% natural abundance). Twenty-one radioisotopes have been characterized, with the most stable being 44Ti with a half-life of 60 years, 45Ti with a half-life of 184.8 minutes, 51Ti with a half-life of 5.76 minutes, and 52Ti with a half-life of 1.7 minutes. All of the remaining radioactive isotopes have half-lives that are less than 33 seconds, and the majority of these have half-lives that are less than half a second. [4]

Contents

The isotopes of titanium range in atomic mass from 39.00  u (39Ti) to 64.00 u (64Ti). The primary decay mode for isotopes lighter than the stable isotopes (lighter than 46Ti) is β+ and the primary mode for the heavier ones (heavier than 50Ti) is β−; their respective decay products are scandium isotopes and the primary products after are vanadium isotopes. [4]

List of isotopes


Nuclide
[n 1] 		Z N Isotopic mass (Da) [5]
[n 2] [n 3] 		Half-life [1]
[n 4] 		Decay
mode [1]
[n 5] 		Daughter
isotope
[n 6] 		Spin and
parity [1]
[n 7] [n 4] 		Natural abundance (mole fraction)
Excitation energyNormal proportion [1] Range of variation
39Ti221739.00268(22)#28.5(9) ms β+, p (93.7%)38Ca3/2+#
β+ (~6.3%)39Sc
β+, 2p (?%)37K
40Ti221839.990345(73)52.4(3) msβ+, p (95.8%)39Ca0+
β+ (4.2%)40Sc
41Ti221940.983148(30)81.9(5) msβ+, p (91.1%)40Ca3/2+
β+ (8.9%)41Sc
42Ti222041.97304937(29)208.3(4) msβ+42Sc0+
43Ti222142.9685284(61)509(5) msβ+43Sc7/2−
43m1Ti313.0(10) keV11.9(3) μs IT 43Ti(3/2+)
43m2Ti3066.4(10) keV556(6) nsIT43Ti(19/2−)
44Ti222243.95968994(75)59.1(3) y EC 44Sc0+
45Ti222344.95812076(90)184.8(5) minβ+45Sc7/2−
45mTi36.53(15) keV3.0(2) μsIT45Ti3/2−
46Ti222445.952626356(97)Stable0+0.0825(3)
47Ti222546.951757491(85)Stable5/2−0.0744(2)
48Ti222647.947940677(79)Stable0+0.7372(3)
49Ti222748.947864391(84)Stable7/2−0.0541(2)
50Ti222849.944785.622(88)Stable0+0.0518(2)
51Ti222950.94660947(52)5.76(1) minβ−51V3/2−
52Ti223051.9468835(29)1.7(1) minβ−52V0+
53Ti223152.9496707(31)32.7(9) sβ−53V(3/2)−
54Ti223253.950892(17)2.1(10) sβ−54V0+
55Ti223354.955091(31)1.3(1) sβ−55V(1/2)−
56Ti223455.95768(11)200(5) msβ−56V0+
57Ti223556.96307(22)95(8) msβ−57V5/2−#
58Ti223657.96681(20)55(6) msβ−58V0+
59Ti223758.97222(32)#28.5(19) msβ−59V5/2−#
59mTi108.5(5) keV615(11) nsIT59Ti1/2−#
60Ti223859.97628(26)22.2(16) msβ−60V0+
61Ti223960.98243(32)#15(4) msβ−61V1/2−#
61m1Ti125.0(5) keV200(28) nsIT61Ti5/2−#
61m2Ti700.1(7) keV354(69) nsIT61Ti9/2+#
62Ti224061.98690(43)#9# ms
[>620 ns]		0+
63Ti224162.99371(54)#10# ms
[>620 ns]		1/2−#
64Ti224263.99841(64)#5# ms
[>620 ns]		0+
This table header & footer:
  1. ↑ mTi – Excited nuclear isomer.
  2. ↑ ( ) – Uncertainty (1σ) is given in concise form in parentheses after the corresponding last digits.
  3. ↑ # – Atomic mass marked #: value and uncertainty derived not from purely experimental data, but at least partly from trends from the Mass Surface (TMS).
  4. 1 2 # – Values marked # are not purely derived from experimental data, but at least partly from trends of neighboring nuclides (TNN).
  5. ↑ Modes of decay:
    EC: Electron capture
    n: Neutron emission
    p: Proton emission
  6. ↑ Bold symbol as daughter – Daughter product is stable.
  7. ↑ ( ) spin value – Indicates spin with weak assignment arguments.

Titanium-44

Titanium-44 (44Ti) is a radioactive isotope of titanium that undergoes electron capture to an excited state of scandium-44 with a half-life of 60 years, before the ground state of 44Sc and ultimately 44Ca are populated. [6] Because titanium-44 can only undergo electron capture, its half-life increases with ionization and it becomes stable in its fully ionized state (that is, having a charge of +22). [7]

Titanium-44 is produced in relative abundance in the alpha process in stellar nucleosynthesis and the early stages of supernova explosions. [8] It is produced when calcium-40 fuses with an alpha particle (helium-4 nucleus) in a star's high-temperature environment; the resulting 44Ti nucleus can then fuse with another alpha particle to form chromium-48. The age of supernovae may be determined through measurements of gamma-ray emissions from titanium-44 and its abundance. [7] It was observed in the Cassiopeia A supernova remnant and SN 1987A at a relatively high concentration, a consequence of delayed decay resulting from ionizing conditions. [6] [7]

Related Research Articles

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There are two natural isotopes of iridium (77Ir), and 37 radioisotopes, the most stable radioisotope being 192Ir with a half-life of 73.83 days, and many nuclear isomers, the most stable of which is 192m2Ir with a half-life of 241 years. All other isomers have half-lives under a year, most under a day. All isotopes of iridium are either radioactive or observationally stable, meaning that they are predicted to be radioactive but no actual decay has been observed.

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<span class="mw-page-title-main">Isotopes of holmium</span>

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Naturally occurring dysprosium (66Dy) is composed of 7 stable isotopes, 156Dy, 158Dy, 160Dy, 161Dy, 162Dy, 163Dy and 164Dy, with 164Dy being the most abundant. Twenty-nine radioisotopes have been characterized, with the most stable being 154Dy with a half-life of 1.4 million years, 159Dy with a half-life of 144.4 days, and 166Dy with a half-life of 81.6 hours. All of the remaining radioactive isotopes have half-lives that are less than 10 hours, and the majority of these have half-lives that are less than 30 seconds. This element also has 12 meta states, with the most stable being 165mDy, 147mDy and 145mDy.

Naturally occurring terbium (65Tb) is composed of one stable isotope, 159Tb. Thirty-seven radioisotopes have been characterized, with the most stable being 158Tb with a half-life of 180 years, 157Tb with a half-life of 71 years, and 160Tb with a half-life of 72.3 days. All of the remaining radioactive isotopes have half-lives that are less than 6.907 days, and the majority of these have half-lives that are less than 24 seconds. This element also has 27 meta states, with the most stable being 156m1Tb, 154m2Tb and 154m1Tb.

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<span class="mw-page-title-main">Isotopes of lanthanum</span>

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Einsteinium (99Es) is a synthetic element, and thus a standard atomic weight cannot be given. Like all synthetic elements, it has no stable isotopes. The first isotope to be discovered was 253Es in 1952. There are 18 known radioisotopes from 240Es to 257Es, and 4 nuclear isomers. The longest-lived isotope is 252Es with a half-life of 471.7 days, or around 1.293 years.

References

  1. 1 2 3 4 5 Kondev, F. G.; Wang, M.; Huang, W. J.; Naimi, S.; Audi, G. (2021). "The NUBASE2020 evaluation of nuclear properties" (PDF). Chinese Physics C. 45 (3): 030001. doi:10.1088/1674-1137/abddae.
  2. ↑ "Standard Atomic Weights: Titanium". CIAAW. 1993.
  3. ↑ Prohaska, Thomas; Irrgeher, Johanna; Benefield, Jacqueline; Böhlke, John K.; Chesson, Lesley A.; Coplen, Tyler B.; Ding, Tiping; Dunn, Philip J. H.; Gröning, Manfred; Holden, Norman E.; Meijer, Harro A. J. (2022-05-04). "Standard atomic weights of the elements 2021 (IUPAC Technical Report)". Pure and Applied Chemistry. doi:10.1515/pac-2019-0603. ISSN   1365-3075.
  4. 1 2 Barbalace, Kenneth L. (2006). "Periodic Table of Elements: Ti - Titanium" . Retrieved 2006-12-26.
  5. ↑ Wang, Meng; Huang, W.J.; Kondev, F.G.; Audi, G.; Naimi, S. (2021). "The AME 2020 atomic mass evaluation (II). Tables, graphs and references*". Chinese Physics C. 45 (3): 030003. doi:10.1088/1674-1137/abddaf.
  6. 1 2 Motizuki, Y.; Kumagai, S. (2004). "Radioactivity of the key isotope 44Ti in SN 1987A". AIP Conference Proceedings. 704 (1): 369–374. arXiv: astro-ph/0312620 . Bibcode:2004AIPC..704..369M. CiteSeerX   10.1.1.315.8412 . doi:10.1063/1.1737130. S2CID   1700673.
  7. 1 2 3 Mochizuki, Y.; Takahashi, K.; Janka, H.-Th.; Hillebrandt, W.; Diehl, R. (2008). "Titanium-44: Its effective decay rate in young supernova remnants, and its abundance in Cas A". Astronomy and Astrophysics. 346 (3): 831–842. arXiv: astro-ph/9904378 .
  8. ↑ Fryer, C.; Dimonte, G.; Ellinger, E.; Hungerford, A.; Kares, B.; Magkotsios, G.; Rockefeller, G.; Timmes, F.; Woodward, P.; Young, P. (2011). Nucleosynthesis in the Universe, Understanding 44Ti (PDF). ADTSC Science Highlights (Report). Los Alamos National Laboratory. pp. 42–43.
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