Nuclear drip line

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The nuclear drip line is the boundary delimiting the zone beyond which atomic nuclei decay by the emission of a proton or neutron.

An arbitrary combination of protons and neutrons does not necessarily yield a stable nucleus. One can think of moving up and/or to the right across the table of nuclides by adding one type of nucleon to a given nucleus. However, adding nucleons one at a time to a given nucleus will eventually lead to a newly formed nucleus that immediately decays by emitting a proton (or neutron). Colloquially speaking, the nucleon has 'leaked' or 'dripped' out of the nucleus, hence giving rise to the term "drip line".

Drip lines are defined for protons, neutrons, and alpha particles, and these all play important roles in nuclear physics. The nucleon drip lines are at the extreme of the proton-to-neutron ratio: at p:n ratios at or beyond the drip lines, no stable nuclei can exist. The location of the neutron drip line is not well known for most of the nuclear chart, whereas the proton and alpha drip lines have been measured for a wide range of elements.

General description[edit]

Nuclear stability is limited to those combinations of protons and neutrons described by the chart of the nuclides, also called the valley of stability. The boundaries of this valley are the neutron drip line on the neutron rich side, and the proton drip line on the proton-rich side.[1] Between those two lines, when a nucleus has a reasonable balance of protons and neutrons, the total nuclear mass is limited by alpha decay, or the alpha drip line, which connects the proton and neutron drip lines. The alpha drip line is somewhat more difficult to visualize as it also branches down through the center of the chart. These limits exist because of particle decay, whereby an exothermic nuclear transition can occur by the emission of one or more nucleons (not to be confused with particle decay in particle physics). As such, the drip line may be defined as the boundary beyond which proton or neutron separation energy becomes negative, favoring the emission of a particle from a newly formed unbound system.[1]

Allowed transitions[edit]

When considering whether a specific nuclear transmutation, a reaction or a decay, is energetically allowed, one only needs to sum the masses of the initial nucleus/nuclei and subtract from that value the sum of the masses of the product particles. If the result, or Q-value, is positive, then the transmutation is allowed, or exothermic because it releases energy, and if the Q-value is a negative quantity, then it is endothermic as at least that much energy must be added to the system before the transmutation may proceed. For example, to determine if 12C, the most common isotope of carbon, can undergo proton emission to 11B, one finds that about 16 MeV must be added to the system for this process to be allowed. While Q-values can be used to describe any nuclear transmutation, for particle decay, the particle separation energy quantity S, is also used, and it is equivalent to the negative of the Q-value. In other words, the proton separation energy Sp indicates how much energy should be added to a given nucleus to remove a single proton. Thus, the particle drip lines defined the boundaries where the particle separation energy is less than or equal to zero, for which the spontaneous emission of that particle is energetically allowed.

Although the location of the drip lines is well defined as the boundary beyond which particle separation energy becomes negative, the definition of what constitutes a nucleus or an unbound resonance is unclear.[1] Some known nuclei of light elements beyond the drip lines decay with lifetimes on the order of 10-22 seconds; this is defined by some to be a limit of nuclear existence as several fundamental nuclear processes occur on this timescale. For more massive nuclei, particle emission half-lives may be significantly longer due to a stronger Coulomb barrier and enable other transitions such as beta decay to instead occur. This renders unambiguous determination of the drip lines difficult, as nuclei with lifetimes long enough to be observed exist far longer than the timescale of particle emission and are most probably bound.[1]

Nuclei near the drip lines are uncommon on Earth[edit]

Of the three types of naturally occurring radioactivities (α, β, and γ), only alpha decay is a type of decay resulting from the nuclear strong force. The other proton and neutron decays occurred much earlier in the life of the atomic species and before the earth was formed. Thus, alpha-decay can be considered either a form of particle decay or, less frequently, as a special case of nuclear fission. The timescale for the nuclear strong force is much faster than that of the nuclear weak force or the electromagnetic force, so the lifetime of nuclei past the drip lines are typically on the order of nanoseconds or less. For alpha decay, the timescale can be much longer than for proton or neutron emission owing to the high Coulomb barrier seen by an alpha-cluster in a nucleus (the alpha particle must tunnel through the barrier). As a consequence, there are no naturally-occurring nuclei on Earth that undergo proton or neutron emission; however, such nuclei can be created, for example, in the laboratory with accelerators or naturally in stars.

Such particle decays are not commonly known because particle decay is governed by the nuclear strong force, as well as the Coulomb force in the case of charged particles, which can act very quickly (femtoseconds or less). In nuclear physics terms, nuclei that are outside the drip lines are particle-unbound and considered not to exist, because they can only exist in the energy continuum rather than in the discrete quantized states we are familiar with. In a discussion of the proton and neutron drip lines, one nomenclatural convenience is to regard beta-unstable nuclei as stable (strictly speaking they are particle-stable), due to the significant difference in the time-scales of these two different decay modes.

Thus, the only type of nuclei that are longer lived and undergo proton or neutron emission are in the class of beta-delayed decays, where first the isospin of one nucleon is reversed (proton to neutron or vice versa) via beta decay, and then if the particle separation energy is non-positive, the daughter nucleus will undergo particle decay. Most naturally occurring γ-sources are technically β-delayed γ-decay, so this concept should be familiar; some gamma-sources are α-delayed but these are generally categorized with other alpha-sources.

Nuclear structure origin of the drip lines[edit]

We can see how the drip lines originate by considering the energy levels in a nucleus. The energy of a nucleon in a nucleus is its rest mass energy minus a binding energy. In addition to this, however, there is an energy due to degeneracy: for instance a nucleon with energy E1 will be forced to a higher energy E2 if all the lower energy states are filled. This is because nucleons are fermions and obey Fermi–Dirac statistics. The work done in putting this nucleon to a higher energy level results in a pressure, which is the degeneracy pressure.

So we can view the energy of a nucleon in a nucleus as its rest mass energy minus an effective binding energy that decreases as we go to higher energy levels. Eventually this effective binding energy has become zero so that the highest occupied energy level, the Fermi energy, is equal to the rest mass of a nucleon. At this point adding a nucleon of the same isospin to the nucleus is not possible, as the new nucleon would have a negative effective binding energy — i.e. it is more energetically favourable (system will have lowest overall energy) for the nucleon to be created outside the nucleus. This is the particle drip point for that species.

Astrophysical relevance[edit]

In nuclear astrophysics the drip lines are especially useful as limiting boundaries for explosive nucleosynthesis as well as other circumstances with extreme pressure or temperature conditions such as neutron stars.


Explosive astrophysical environments often have very large fluxes of high energy nucleons that can be captured on seed nuclei. In these environments, radiative proton or neutron capture will occur much faster than beta decays, and as astrophysical environments with both large neutron fluxes and high energy protons are unknown at present, the reaction flow will proceed away from beta-stability towards or up to either the neutron or proton drip lines, respectively. However, once a nucleus reaches a drip line, as we have seen, no more nucleons of that species can be added to the particular nucleus, and the nucleus must first undergo a beta decay before further nucleon captures can occur.


While the drip lines impose the ultimate boundaries for nucleosynthesis, in high energy environments the burning pathway may be limited before the drip lines are reached by photodisintegration, where a high energy gamma ray knocks a nucleon out of a nucleus. The same nucleus is subject both to a flux of nucleons and photons, so an equilibrium is reached where mass builds up at particular nuclear species.

As the photon bath will typically be described by a Planckian distribution, higher energy photons will be less abundant, and so photodisintegration will not become significant until the nucleon separation energy begins to approach zero towards the drip lines, where photodisintegration may be induced by lower energy gamma rays. At 1 × 109 Kelvin, the photon distribution is energetic enough to knock nucleons out of any nuclei that have particle separation energies less than 3 MeV,[2] but to know which nuclei exist in what abundances one must also consider the competing radiative captures.

As neutron captures can proceed in any energy regime, neutron photodisintegration is unimportant except at higher energies. However, as proton captures are inhibited by the Coulomb barrier, the cross sections for those charged-particle reactions at lower energies are greatly suppressed, and in the higher energy regimes where proton captures have a large probability to occur, there is often a competition between the proton capture and the photodisintegration that occurs in explosive hydrogen burning; but because the proton drip line is relatively much closer to the valley of beta-stability than is the neutron drip line, nucleosynthesis in some environments may proceed as far as either nucleon drip line.

Waiting points and time scales[edit]

Once radiative capture can no longer proceed on a given nucleus, either from photodisintegration or the drip lines, further nuclear processing to higher mass must either bypass this nucleus by undergoing a reaction with a heavier nucleus such as 4He, or more often wait for the beta decay. Nuclear species where a significant fraction of the mass builds up during a particular nucleosynthesis episode are considered nuclear waiting points, since further processing by fast radiative captures is delayed.

As has been emphasized, the beta decays are the slowest processes occurring in explosive nucleosynthesis. From the nuclear physics side, explosive nucleosynthesis time scales are set simply by summing the beta decay half-lives involved,[3] since the time scale for other nuclear processes is negligible in comparison, although practically speaking this time scale is typically dominated by the sum of a handful of waiting point nuclear half lives.

The r-process[edit]

The rapid neutron capture process probably operates very close to the neutron drip line. Thus, the reaction flow in the r-process is generally assumed to run along the neutron drip line. However, the astrophysical site of the r-process, while widely believed to take place in core-collapse supernovae, is unknown. Furthermore, the neutron drip line is very poorly determined experimentally, and nuclear mass models give various predictions for the precise location of the neutron drip line. In fact, the nuclear physics of extremely neutron-rich matter is a fairly new subject, and already has led to the discovery of the island of inversion and halo nuclei such as 11Li, which has a very diffuse neutron skin leading to a total radius comparable to that of 208Pb.[clarification needed] Thus, although the neutron drip line and the r-process are linked very closely in research, it is an unknown frontier awaiting future research, both from theory and experiment.

The rp-process[edit]

The rapid proton capture process in X-ray bursts runs at the proton drip line except near some photodisintegration waiting points. This includes the nuclei 21Mg, 30S, 34Ar, 38Ca, 56Ni, 60Zn, 64Ge, 68Se, 72Kr, 76Sr, and 80Zr.[4][5]

One clear nuclear structure pattern that emerges is the importance of pairing, as one notices all the waiting points above are at nuclei with an even number of protons, and all but 21Mg also have an even number of neutrons. However, the waiting points will depend on the assumptions of the X-ray burst model, such as metallicity, accretion rate, and the hydrodynamics, along with the nuclear uncertainties, and as mentioned above, the exact definition of the waiting point may not be consistent from one study to the next. Although there are nuclear uncertainties, compared to other explosive nucleosynthesis processes, the rp-process is quite well experimentally constrained, as, for example, all the above waiting point nuclei have at the least been observed in the laboratory. Thus as the nuclear physics inputs can be found in the literature or data compilations, the Computational Infrastructure for Nuclear Astrophysics allows one to do post-processing calculations on various X-ray burst models, and define for oneself the criteria for the waiting point, as well as alter any nuclear parameters.

While the rp-process in X-ray bursts may have difficulty by-passing the 64Ge waiting point,[5] certainly in X-ray pulsars where the rp-process is stable, the alpha drip line places an upper limit near A=100 on the mass that can be reached through continuous burning;[6] the exact location of the alpha drip line is a matter presently under investigation, and 106Te is known to alpha-decay whereas 103Sb is particle-bound. However, it has been shown that if there are episodes of cooling or mixing of previous ashes into the burning zone, material as heavy as 126Xe can be created.[7]

Neutron stars[edit]

In neutron stars, neutron heavy nuclei are found as relativistic electrons penetrate the nuclei and produce inverse beta decay, wherein the electron combines with a proton in the nucleus to make a neutron and an electron-neutrino:




As more and more neutrons are created in nuclei the energy levels for neutrons get filled up to an energy level equal to the rest mass of a neutron. At this point any electron penetrating a nucleus will create a neutron, which will "drip" out of the nucleus. At this point we have:

And from this point onwards the equation

applies, where pFn is the Fermi momentum of the neutron. As we go deeper into the neutron star the free neutron density increases, and as the Fermi momentum increases with increasing density, the Fermi energy increases, so that energy levels lower than the top level reach neutron drip and more and more neutrons drip out of nuclei so that we get nuclei in a neutron fluid. Eventually all the neutrons drip out of nuclei and we have reached the neutron fluid interior of the neutron star.

Known values[edit]

Neutron drip line[edit]

The values of the neutron drip line are only known for the first ten elements, hydrogen to neon.[8] For oxygen (Z = 8), the maximal number of bound neutrons is 16, rendering 24O the heaviest particle-bound oxygen isotope.[9] For neon (Z = 10), the maximal number of bound neutrons increases to 24, rendering 34Ne the heaviest particle-bound neon isotope. The drip line for fluorine and neon was determined in 2017 by the non-observation of the two isotopes located immediately beyond the drip line; this was the first new discovery along the neutron drip line in over twenty years.[10]

The neutron drip line is expected to diverge from the line of beta stability after calcium with an average neutron-to-proton ratio of 2.4.[1] Hence, is predicted that the neutron drip line will fall out of reach for elements beyond zinc (N = 60) or possibly zirconium (N = 88), as no known experimental techniques are theoretically capable of creating the necessary imbalance of protons and neutrons in drip line isotopes of heavier elements.[1]

The table below lists the heaviest particle-bound isotope of the first ten elements.[11]

Z Species
01 03H
02 08He
03 011Li
04 014Be
05 017B
06 022C
07 023N
08 024O
09 031F
010 034Ne

Proton drip line[edit]

The general location of the proton drip line is well established. For all elements occurring naturally on earth and having an odd number of protons, at least one species with a proton separation energy less than zero has been experimentally observed. Up to germanium the location of the drip line for many elements with an even number of protons is known, but none past that point are listed in the evaluated nuclear data. There are a few exceptional cases where, due to nuclear pairing, there are some particle-bound species outside the drip line, such as 8B and 178Au[verification needed]. One may also note that nearing the magic numbers, the drip line is less understood. A compilation of the known first unbound nuclei beyond the proton drip line is given below, with the number of protons, Z and the corresponding isotopes, taken from the National Nuclear Data Center.[12]

Z Species
02 02He
03 05Li
04 05Be
05 07B, 09B
07 11N
08 12O
09 16F
11 19Na
12 19Mg
13 21Al
15 25P
17 30Cl
19 34K
21 39Sc
23 42V
25 45Mn
27 50Co
29 55Cu
31 59Ga
32 58Ge
33 65As
35 69Br
37 73Rb
39 77Y
41 81Nb
43 85Tc
45 89Rh
47 93Ag
49 97In
51 105Sb
53 110I
55 115Cs
57 119La
59 123Pr
61 128Pm
63 134Eu
65 139Tb
67 145Ho
69 149Tm
71 155Lu
73 159Ta
75 165Re
77 171Ir
79 175Au, 177Au
81 181Tl
83 189Bi
85 195At
87 201Fr
89 207Ac
91 214Pa

See also[edit]


  1. ^ a b c d e f Thoennessen, M. (2004). "Reaching the limits of nuclear stability" (PDF). Reports on Progress in Physics. 67: 1187–1232. doi:10.1088/0034-4885/67/7/R04.
  2. ^ Thielemann, Friedrich-Karl; Kratz, Karl-Ludwig; Pfeiffer, Bernd; Rauscher, Thomas; et al. (1994). "Astrophysics and nuclei far from stability". Nuclear Physics A. 570 (1–2): 329. Bibcode:1994NuPhA.570..329T. doi:10.1016/0375-9474(94)90299-2.
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  4. ^ Koike, O.; Hashimoto, M.; Arai, K.; Wanajo, S. (1999). "Rapid proton capture on accreting neutron stars – effects of uncertainty in the nuclear process". Astronomy and Astrophysics. 342: 464. Bibcode:1999A&A...342..464K.
  5. ^ a b Fisker, Jacob Lund; Schatz, Hendrik; Thielemann, Friedrich-Karl (2008). "Explosive Hydrogen Burning during Type I X-Ray Bursts". The Astrophysical Journal Supplement Series. 174 (1): 261. arXiv:astro-ph/0703311. Bibcode:2008ApJS..174..261F. doi:10.1086/521104.
  6. ^ Schatz, H.; A. Aprahamian; V. Barnard; L. Bildsten; et al. (April 2001). "End Point of the rp Process on Accreting Neutron Stars" (subscription required). Physical Review Letters. 86 (16): 3471–3474. arXiv:astro-ph/0102418. Bibcode:2001PhRvL..86.3471S. doi:10.1103/PhysRevLett.86.3471. PMID 11328001. Retrieved 2006-08-24.
  7. ^ Koike, Osamu; Hashimoto, Masa-aki; Kuromizu, Reiko; Fujimoto, Shin-ichirou (2004). "Final Products of the rp-Process on Accreting Neutron Stars". The Astrophysical Journal. 603 (1): 242–251. Bibcode:2004ApJ...603..242K. doi:10.1086/381354. (Subscription required (help)).
  8. ^ "Three First-ever Atomic Nuclei Created; New Super-heavy Aluminum Isotopes May Exist". 2007-10-27. Retrieved 2010-04-06.
  9. ^ "Nuclear Physicists Examine Oxygen's Limits". 2007-09-18. Retrieved 2010-04-06.
  10. ^ Tarasov, O.B. (2017). "Production of very neutron rich isotopes: What should we know?".
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  12. ^ "National Nuclear Data Center". Retrieved 2010-04-13.