Isomerism in the “south-east” of {}^{132}Sn and a predicted neutron-decaying isomer in {}^{129}Pd

Isomerism in the “south-east” of Sn and a predicted neutron-decaying isomer in Pd

Abstract

Excited states in neutron-rich nuclei located south-east of Sn are investigated by shell-model calculations. A new shell-model Hamiltonian is constructed for the present study. The proton-proton and neutron-neutron interactions of the Hamiltonian are obtained through the existing CD-Bonn matrix results, while the proton-neutron interaction across two major shells is derived from the monopole based universal interaction plus the M3Y spin-orbit force. The present Hamiltonian can reproduce well the experimental data available in this region, including one-neutron separation energies, level energies and the experimental values of isomers in Sn, Cd, and Pd. New isomers are predicted in this region, in Sn, Cd, Pd, In and Ag, in which almost no excited states are known experimentally yet. In the odd-odd In and Ag, the predicted very long life-times of the low-lying states are discussed, demanding more information on the related proton-neutron interaction. The low-lying states of In are discussed in connection with the recently observed rays. The predicted isomer in Pd could decay by both electromagnetic transitions and neutron emission with comparable partial life-times, making it a good candidate for neutron radioactivity, a decay mode which is yet to be discovered.

keywords:
1

1 Introduction

On the journey towards the neutron drip-line one needs a reliable theoretical model which incorporates the known features of the nuclear many-body system and has enough predictive power for a range of unexplored nuclei. The nuclear shell model is one such, providing the basic framework for understanding the detailed structure of complex nuclei as arising from the individual motion of nucleons and the effective nuclear interactions between them. In the shell model, doubly magic nuclei, especially those far from the line of stability, such as Sn, act as cornerstones for exploring the unknown regions.

Experimentally, the observation of isomers has been key to the understanding of the shell structure and the development of the shell model segre1949 (). Recently, nuclei around Sn have been the subject of intensive experimental studies with respect to the persistence of the shell gap and its relevance to the astrophysical -process path. Early -decay results seemed to indicate a substantial shell quenching dillmann2003 (), while isomeric spectroscopy studies gave evidence for the persistence of the shell down to , Pd jungclaus2007 (); gorska2009 (); watanabe2013 (). Along the line isomeric states were also observed in Sn korgul2000 (); simpson2014 (), and mixing between seniority-2 and -4 configurations was revealed for the isomer of Sn simpson2014 (). Furthermore, mass measurements have been crucial for experimental determination of the shell gaps At15 (); Kn16 ().

In addition, isomers in the region far from the -stability line could serve as stepping stones towards the drip-lines. For example, the high-spin isomer in Co provided the first example of proton radioactivity jackson1970 (). Similarly in the very neutron-rich region, a neutron may “drip” from an isomer before the neutron drip-line itself is reached, if the isomer’s excitation energy takes it above the neutron separation energy Pe71 (); walker2006 ().

In this paper, shell-model calculations are performed to investigate the isomerism in the south-east quadrant of Sn, i.e. with and , including the possibility of neutron radioactivity from such isomers.

2 Effective Hamiltonian

The construction of an effective Hamiltonian is one of the key elements in a shell-model study. The model space for the present work is , , , , and , , , , , , corresponding to the and major shells, respectively. Below Sn, the robustness of the shell gap has been experimentally examined and confirmed down to Cd and Pd jungclaus2007 (); watanabe2013 (); At15 (); Kn16 (). The core excited states in In are found to be at nearly 4 MeV gorska2009 (), thus this model space is suitable for the investigation of the low-lying states around or lower than 2 MeV in Sn, In, Cd, Ag, and Pd isotopes with . So far there is no well established effective Hamiltonian for this model space due to the lack of experimental data on the excited states in this most neutron-rich region around Sn. An effective Hamiltonian for this model space is proposed below. In a very recent work, shell-model calculations for In were performed employing a modern realistic effective interaction and two-body matrix elements deduced from the Pb region Jungclaus2016 ().

The single-particle energies for the four proton orbits and the six neutron orbits in the present model space are fitted to the reported energies of the single-particle states of In and Sn, respectively. These energies are from Ref. nndc () and the recently discovered and single-hole states in In Kankainen2013 (); taprogge2014 (). The single-particle energy for the orbit in Ref. nndc () is estimated from the excitation energy of the state in Sb  Urban1999 (). The present Hamiltonian fixes the relative single-particle energies to the observed excited states. It is reasonable as the present work concentrates on the excitation energies of levels and neutron separation energies.

The proton-proton interaction is based on the proton-proton part of jj45pna Hamiltonian, which has been derived from the CD-Bonn potential through the matrix renormalization method by Hjorth-Jensen and is included in the OXBASH package OXBASH (). The theoretical method to derive the jj45pna effective interaction and its application in the region is described in Ref. Jensen1995 (). Recently, the Hamiltonian jj45pna was also used to investigate the decay of Cd and In Haaranen2016 (), and the low-lying states of In isotopes around A=125 Rejmund2016 (). The strength of this interaction is modified by a factor to reproduce the low-lying states of Cd. The neutron-neutron interaction is from the neutron-neutron part of CWG Hamiltonian, which is derived from the CD-Bonn renormalized matrix and used to study nuclei around Sn brown2005 ().

The proton-neutron interaction is calculated through an effective nucleon-nucleon, monopole-based universal interaction V otsuka2010 () plus a spin-orbit force from M3Y m3y1977 ()(V+LS). The validity of the V+LS interaction in shell-model calculations has been examined in different regions of the chart of nuclei. The structure features of neutron rich C, N, O yuan2012 (), Si, S, Ar, Ca utsuno2012 (), Cr, and Fe isotopes Togashi2015 () have been nicely described by shell-model calculations by taking V+LS as the proton-neutron interaction between the proton shell and the neutron shell yuan2012 (), the proton shell and the neutron shell utsuno2012 (), and the proton shell and the neutron shell Togashi2015 (), respectively. For example, the neutron drip-lines for carbon, nitrogen and oxygen isotopes are simultaneously explained, revealing the impact of the proton-neutron interaction on the evolution of the nuclear shell yuan2012 (). Recently, the first state of S has been identified as a high- isomer Utsuno2015 () through the Hamiltonian suggested in Ref. utsuno2012 (). In the heavier region, close to Sn, the change of the energy difference between the and yrast levels in the isotones down to Pd is well explained by V+LS Watanabe2014 (). Thus it is natural and reasonable to use this interaction as the proton-neutron interaction in the present study.

In the present Hamiltonian the strength of the central-force parameters of V is enhanced times the original one in Ref. otsuka2010 () to give a better description of the one-neutron separation energies . It should be noted that the original form of V comes from the effective Hamiltonian in the and regions. In region, the strength of its central part is reduced by a factor of to reproduce the binding energies of the B, C, N, and O isotopes. The new Hamiltonian is named as in the following discussion as it includes 4 and 6 valence proton and neutron orbits, respectively. The present shell-model calculations are performed using the code OXBASH OXBASH ().

It should be mentioned that the present Hamiltonian operates in the particle-particle model space. The doubly magic nucleus Sn has fully occupied valence protons and no valence neutrons in the present model space. Starting from Sn, the proton-hole energies of In and the neutron-particle energies of Sn are not directly taken as the single particle energies in the Hamiltonian, but are modified by the residual proton-proton and proton-neutron interactions, respectively. The proton-hole states in the present work are affected by the missing correlations due to the removal of protons from the fully occupied - shell. In the following discussion, the configurations are written in the proton-hole neutron-particle scheme for simplicity.

3 Results and Discussion

Nuclei
Sn 2.402(4) 2.408 2.651
Sn 3.629(4) 3.732 4.281
Sn 2.271(4) 2.405 1.871
Sn 3.795 3.340 3.741
Sn 2.339 1.960 1.611
Sn 3.834 3.140 3.561
In 2.450(60) 2.364 2.701
In 3.418 3.130 3.781
In 2.370 2.270 1.771
Cd 2.169(103) 1.984 1.870 2.031
Cd 3.324 3.000 3.671
Cd 1.977 1.730 1.321
Ag 1.902 1.780 2.001
Pd 1.524 1.461
Table 1: One neutron separation energies of experiments from Ref audi2012 () except Cd from At15 (), predictions of AME2012 audi2012 (), calculations through the finite range liquid drop model  moller1995 () and the present work . (All values are in MeV.)

With the Hamiltonian described above, the properties of Sn, In, Cd, Ag, and Pd are investigated. One-neutron separation energies calculated using the present Hamiltonian are listed in Table 1 together with the predictions of AME2012 audi2012 (), the finite range droplet model (FRDM) moller1995 () results, and experimental values available. The present calculations reproduce the few experimental neutron separation energies audi2012 () in this region nicely. Both the single-particle energy of the orbit and the proton-neutron interactions involving the fully occupied proton orbits contribute to of Sn. Its value together with the other observed values are used to constrain the strength of the proton-neutron interaction in the present Hamiltonian as discussed in the previous section.

Figure 1: Comparison between the calculated levels in Sn in the present work and those observed experimentally simpson2014 (); nndc ().
Figure 2: Calculated neutron effective single-particle energies (ESPE) for Sn isotopes (Color online).

The levels of neutron-rich Sn isotopes are presented in Fig. 1. The present Hamiltonian reproduces the known low-lying states of Sn well, especially the positions of the states in Sn and the increasing trend of the energies of and states from Sn to Sn. The dominant configurations of the states in Sn and Sn are 99.55% and 41.83% , respectively. This state in Sn is dominated by the configuration (84.34%). If all the yrast and levels in Sn were dominated by a pure seniority-2 configuration, the value in Sn would be expected to be the lowest among these three isotopes, but their experimental results are decreasing from Sn to Sn. The seniority scheme of the low-lying states in these three isotopes can be discussed through the comparison between the experimental results and the shell model calculations. The observed value indicates a mixing of seniority-2 and -4 configurations in the state of Sn by comparing the results from a realistic effective interaction and the empirical modification of matrix elements simpson2014 (); Maheshwari2015 (). The present calculation also gives the decreasing values between and states from Sn to Sn, which will be shown later.

The large energy differences between the and states in these three nuclei suggest that the states are not isomeric. However the small energy difference between the and states in Sn implies a metastable state. Details for this possible isomer in Sn will be given later. However, no such isomer is predicted in Sn (not shown in Fig. 1). The first state of Sn is dominated by a configuration (96.7%). Compared with Sn the first level in Sn is expected to be more mixed because of the increasing number of valence neutrons and/or the change of the shell structure. Fig. 2 presents the effective single-particle energies (ESPE) of the neutron orbits in Sn isotopes. ESPE are defined as otsuka20012 (),

(1)

where is the single-particle energy relative to the core, is the shell-model occupancy of the orbit and is the monopole part of the two-body interaction. As shown in Fig. 2, the single particle energies do not change much in the Sn isotopes. Therefore the main difference between the states in Sn and Sn arises from the two additional valence neutrons in Sn. The configuration of the first level in Sn is a mixture of (61.3%), (9.97%), (9.05%), and (3.38%), very different from the almost pure configuration in Sn.

Figure 3: The same as Fig. 1, but for In, Cd, and Pd.
Figure 4: Calculated excitation energies of the multiplets in In as function of spin.
Figure 5: Proton hole and neutron particle ESPEs for isotones calculated in the present work (Color online).

Levels of the In, Cd, and Pd isotopes are presented in Fig. 3. Some of them are possibly isomers. The ground state of In is found to be with a configuration of , in agreement with the experimental assignment nndc (). Our calculations indicate a very low state in In, which can be a candidate for an isomer. With two more neutrons and two more proton holes respectively, In and Ag have similar structure, for ground state and very low for first excited state. These results depend on the details of the proton-neutron interaction between and orbits, for which the experimental information is still rare.

Recently six rays were observed following the -delayed neutron emission from Cd and assumed to be emitted from the excited states of In Jungclaus2016 (). Due to the low statistics and the lack of - coincidence, it was difficult to establish a level scheme with those observed rays Jungclaus2016 (). The spin parity of the ground state of Cd is from Ref. nndc () and the present shell-model calculation. As the decay energy ( MeV) of Cd is much larger than the neutron separation energy ( MeV) of In, the ground state of Cd can decay to many high excited states beyond the neutron emission threshold of In, with spin parity to through Gamow-Teller transitions and to through first forbidden transitions. Thus many states in In could be populated in the -delayed neutron emission of Cd.

The low-lying states of the configurations in In calculated by the present Hamiltonian are shown in Fig. 4. The present shell-model results are similar to those shown in Fig. 4(a) of Ref. Jungclaus2016 (), especially for the , , and multiplets, though the proton-neutron interaction is calculated through V+LS in this work, while it is derived from the CD-Bonn potential with V approach in Jungclaus2016 ().

In both calculations the state is the lowest and the highest among the multiplets, however the other states are slightly different. The present work predicts that is first excited state and a little lower than state, while the shell-model calculation in Ref. Jungclaus2016 () gave opposite prediction. Similarly the present shell-model results may also explain most of the observed rays in In Jungclaus2016 (). Because of the uncertainty of the shell-model calculations and extra complexity introduced by the low-lying multiplets, more experimental information on the excited states of In, In and Ag are highly desired and crucial in understanding the proton-neutron interactions in this region.

The ESPE for proton-hole and neutron-particle orbits along the closed shell are shown in Fig. 5, where it can be seen that the and proton orbits are quite close to each other. So the states in odd-Z N=82 isotones are predicted to be the first excited state beyond ground state and are long-lived isomers, consistently with the experimental observation that in both In and Ag the low-lying states are -decaying isomers  Kankainen2013 (); nndc (). The ground state of Cd is found to be a mixture of and . The low-lying positive-parity states of Cd are formed through the coupling of . The present calculations show that the and states of Cd are dominated by the configuration with 93.0% and 99.2%, respectively. The contribution from other configurations such as , , or , is very small as they have much higher energies. In the present model space, the and states can only be formed from the configuration. Previous shell-model work showed similar results grawe2004 () for Cd. As expected from the seniority scheme, the yrast state in Cd was found to be isomeric jungclaus2007 (). Similarly the seniority isomer in Pd was recently identified at RIKEN watanabe2013 ().

Nuclei Configuration
Sn 1.267 0.149 41.72 0.266 35(6) (96.3%)
Sn 2.288 0.147 93.96 0.127 (96.7%)
Sn 1.388 0.222 15.43 0.098 24(4) (75.5%)
Sn 1.544 0.183 12.80 0.311 19(4) (53.13%)
In 0.067 0.067 1.75 345.7 (99.0%)
In 0.972 0.257 48.36 0.015 (93.9%)
In 0.074 0.074 27.69 13.28 (72.5%)
Cd 2.109 0.106 59.07 1.032 66(13)/50(10) (100.0%)
Cd 1.778 0.140 100.03 0.152 (99.7%)
Ag 0.072 0.072 18.72 22.53 (74.3%)
Pd 2.186 0.099 12.50 6.866 8.43(0.25) (71.1%)
Pd 1.903 0.146 12.88 0.955 (74.2%)
Pd 1.328 0.213 185.41 0.010 (54.6%)
Table 2: Excitation energies (MeV), transition energies (MeV), observed jungclaus2007 (); watanabe2013 (); simpson2014 () and calculated values (), calculated mean life-time (), and the dominant configurations for possible isomeric states.

All the seniority isomers experimentally observed in Sn, Cd and Pd are well reproduced. Their semi-magic nature validates the neutron-neutron and proton-proton parts of the shell-model interactions in the present work. In some other nuclei in this region, some of the levels are possibly isomeric because of the slow transition rates resulting from low transition energies. These isomer candidates are listed in Table 2 together with those experimentally confirmed in Sn isotopes and N=82 isotones. is the mean life-time of transitions obtained from the theoretical reduced transition probability values and predicted transition energies. The experimental values of Sn are from Ref. simpson2014 (). The two values of Cd are due to the two possible decay transition energies jungclaus2007 (). The effective charges for calculation of values for protons and neutrons are and , respectively, which are similar to those used in Ref. simpson2014 ().

The isomer in Sn is analogous to the isomer in Sn, but its value is much larger than that of Sn, as shown in Table. 2. The one-body transition density of the neutron orbit from to in Sn is almost the same as that from to in Sn, and the enhancement in Sn is mainly due to the transition from to and to . Although the occupancies of and in the state are small, the large number of and particles in the state result in a large one-body transition density. The transition energy between and in Sn is predicted to be almost the same as that between and in Sn. around ns is predicted for the isomer in Sn.

The yrast states in In and Ag are predicted to be closely below the levels and only around keV above the ground states, as shown in Fig. 4 for In, leading to long life-times. A much larger in In is predicted because of the small value caused by the cancellation between the proton and neutron contributions. It should be noted that due to the lack of experimental information on the proton-neutron interaction in this quadrant of Sn, large uncertainties related to the isomerism in these odd-odd nuclei are not unexpected in the present shell-model calculations. For example, the isomer will disappear if it is higher than the state. Or alternatively the state could be isomeric, if it lies below the state.

isomers are predicted in the isotones Cd and Pd, with ns and s, respectively. The excitation energy of the predicted isomer in Pd is around MeV above its neutron separation energies predicted by the present work and by Moller et al. moller1995 () (Table 1) and so it may decay to the ground state of Pd by emitting a neutron with an orbital angular momentum of = 9 (not to state of Pd because of its MeV excitation energy). The half-life of neutron emission is calculated by using the widely-used formula of the two-potential approach Gurvitz1987 (), in which both the pre-exponential factor and exponential factor are explicitly defined. The potential that the emitted neutron feels is a sum of the nuclear potential, the spin-orbit potential and the centrifugl potential. The form of both the Woods-Saxon nuclear potential and the spin-orbit potential and the parameters used are taken from textbook Nilsson1995 (),

(2)

where , fm, fm, , , and is the average mass of a nucleon. The depth of the nuclear potential is determined by the Bohr-Sommerfeld condition to ensure a quasi-bound state Xu2006 (),

(3)

where is the reduced mass of the neutron, is the decay energy, and are classical turning points defined by , and is the global quantum number. The predicted life-time for neutron emission from the state of Pd to the ground state of Pd ranges from to s with the decay energy = 0.35-0.50 MeV, comparable to that of the calculated electromagnetic decay. The global quantum number in the Bohr-Sommerfeld condition is fixed at 9 due to the very low decay energy.

4 Summary

In summary, a shell-model study has been performed in the south-east of Sn to search for possible isomeric states. A new shell-model Hamiltonian has been constructed for the present investigation. The proton-proton and neutron-neutron interactions, which are each limited to one major shell, have been obtained from existing CD-Bonn matrix calculations. The proton-neutron interaction across two major shells is calculated through the V plus M3Y spin-orbit interaction. The present Hamiltonian, , is able to reproduce well the one-neutron separation energies, level energies, and values of the already observed isomers in this region. New isomeric states are predicted and their structures are discussed. The predicted isomer in Pd could be a candidate for neutron radioactivity.

5 Acknowledgements

This work has been supported by the National Natural Science Foundation of China under Grant Nos. 11235001, 11305272, 11375086, 11405224, 11435014, 11575007, 11535004, and 11320101004, the Special Program for Applied Research on Super Computation of the NSFC Guangdong Joint Fund (the second phase), the Specialized Research Fund for the Doctoral Program of Higher Education under Grant No. 20130171120014, the Guangdong Natural Science Foundation under Grant No. 2014A030313217, the Fundamental Research Funds for the Central Universities under Grant No. 14lgpy29, the Pearl River S&T Nova Program of Guangzhou under Grant No. 201506010060 and Hundred-Talent Program (Chinese Academy of Sciences), and the United Kingdom Science and Technology Facilities Council under grant No. ST/L005743/1.

Footnotes

  1. journal: Physics Letters B

References

  1. E. Segre and A.C. Helmholz, Rev. Mod. Phys. 21 271 (1949).
  2. I. Dillmann et al., Phys. Rev. Lett. 91, 162503 (2003).
  3. A. Jungclaus, et al., Phys. Rev. Lett. 99, 132501 (2007).
  4. M. Grska, et al., Phys. Lett. B 672, 313 (2009).
  5. H. Watanabe, et al., Phys. Rev. Lett. 111, 152501 (2013).
  6. A. Korgul, et al., Eur. Phys. J. A 7, 167 (2000).
  7. G.S. Simpson, et al., Phys. Rev. Lett. 113, 132502 (2014).
  8. D. Atanasov, et al., Phys. Rev. Lett. 115, 232501 (2015).
  9. R. Knöbel, et al., Phys. Lett. B 754, 288(2016).
  10. K.P. Jackson et al., Phys. Lett. B 33, 281 (1970).
  11. L.K. Peker, et al., Phys. Lett. B 36, 547 (1971).
  12. P.M. Walker, AIP Conf. Proc. 819, 16 (2006).
  13. A. Jungclaus, et al., Phys Rev. C 93, 041301(R) (2016).
  14. http://www.nndc.bnl.gov/nudat2/
  15. A. Kankainen, et al., Phys Rev. C 87, 024307 (2013).
  16. J. Taprogge, et al., Phys. Rev. Lett. 112, 132501 (2014).
  17. W. Urban, et al., Eur. Phys. J. A 5, 239 (1999).
  18. OXBASH, the Oxford, Buenos-Aires, Michigan State, Shell Model Program, B.A. Brown, A. Etchegoyan, and W.D.M. Rae, MSU Cyclotron Laboratory Report No. 524, 1986.
  19. M. Hjorth-Jensen, T.T.S. Kuo, and E. Osnes, Phys. Rep. 261, 125 (1995); A. Holt, T. Engeland, M. Hjorth-Jensen, and E. Osnes, Phys. Rev. C 61, 064318 (2000); Engeland, M. Hjorth-Jensen, and E. Osnes, Phys. Rev. C 61, 021302(R) (2000).
  20. M. Haaranen, P.C. Srivastava, and J. Suhonen, Phys Rev. C 93, 034308 (2016).
  21. M. Rejmund et al., Phys. Lett. B 753, 86 (2016).
  22. B.A. Brown, N.J. Stone, J.R. Stone, I.S. Towner, and M. Hjorth-Jensen, Phys Rev. C 71, 044317 (2005).
  23. T. Otsuka, T. Suzuki, M. Honma, Y. Utsuno, N. Tsunoda, K. Tsukiyama, and M. Hjorth-Jensen, Phys. Rev. Lett. 104, 012501 (2010).
  24. G. Bertsch, J. Borysowicz, H. McManus, and W. G. Love, Nucl. Phys. A284, 399 (1977).
  25. C.X. Yuan, T. Suzuki, T. Otsuka, F.R. Xu, and N. Tsunoda, Phys Rev. C 85, 064324 (2012).
  26. Y. Utsuno, T. Otsuka, B. A. Brown, M. Honma, T. Mizusaki, and N. Shimizu, Phys Rev. C 86, 051301(R) (2012).
  27. T. Togashi, N. Shimizu, Y. Utsuno, T. Otsuka, and M. Honma, Phys Rev. C 91, 024320 (2015).
  28. Y. Utsuno, N. Shimizu, T. Otsuka, T. Yoshida, and Y. Tsunoda, Phys. Rev. Lett. 114, 032501 (2015).
  29. H. Watanabe, et al., Phys. Rev. Lett. 113, 042502 (2014).
  30. M. Wang, et al., Chin. Phys. C 36(12), 1603 (2012).
  31. T. Otsuka, M. Honma, T. Mizusaki, N. Shimizu, and Y. Utsuno Prog. Part. Nucl. Phys. 47,319 (2001).
  32. P. Möller, J.R. Nix, W. D. Myers, and W. J. Swiatecki, At. Data Nucl. Data Tables 59, 185 (1995).
  33. B. Maheshwari, A.K. Jain, and P.C. Srivastava, Phys Rev. C 91, 024321 (2015).
  34. H. Grawe, Lect. Notes Phys. 651, 33 (2004).
  35. S.A. Gurvitz and G. Kalbermann, Phys. Rev. Lett. 59, 262 (1987).
  36. S.G. Nilsson and I. Ragnarsson, Shapes and Shells in Nuclear Structure (Cambridge University Press, 1995).
  37. C. Xu and Z.Z. Ren, Phys. Rev. C 74, 014304 (2006).
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
""
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
   
Add comment
Cancel
Loading ...
148198
This is a comment super asjknd jkasnjk adsnkj
Upvote
Downvote
""
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters
Submit
Cancel

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test
Test description