Adolescent substance use in the context of the family: a qualitative study of young people’s views on parent-child attachments, parenting style and parental substance use

Background: Adolescent substance use can place youth at risk of a range of poor outcomes. Few studies have attempted to explore in-depth young people’s perceptions of how familial processes and dynamics influence adolescent substance use.
Objectives: This paper aimed to explore risk and protective factors for youth substance use within the context of the family with a view to informing family based interventions.
Methods: Nine focus groups supplemented with participatory techniques were facilitated with a purposive sample of sixty-two young people (age 13-17 years) from post-primary schools across Northern Ireland. The data were transcribed verbatim and analysed using thematic analysis.
Results: Three themes emerged from the data: 1) parent-child attachments, 2) parenting style and 3) parental and sibling substance misuse. Parent-child attachment was identified as an important factor in protecting adolescents from substance use in addition to effective parenting particularly an authoritative style supplemented with parental monitoring and strong parent-child communication to encourage child disclosure. Family substance use was considered to impact on children’s substance use if exposed at an early age and the harms associated with parental substance misuse were discussed in detail. Both parent and child gender differences were cross-cutting themes.
Conclusion: Parenting programmes (tailored to mothers and fathers) may benefit young people via components on authoritative styles, parental monitoring, communication, nurturing attachments and parent-child conflict. Youth living with more complex issues, e.g. parental substance misuse, may benefit from programmes delivered beyond the family environment e.g. school based settings.

Photoionization of Costyle="margin: 0px; padding: 0px; border: 0px; outline-style: none; font-weight: inherit; font-style: inherit; font-size: 0.85em; font-family: inherit; line-height: 0; text-align: inherit;">+ and electron-impact excitation of Costyle="margin: 0px; padding: 0px; border: 0px; outline-style: none; font-weight: inherit; font-style: inherit; font-size: 0.85em; font-family: inherit; line-height: 0; text-align: inherit;">2 + using the Dirac style="margin: 0px; padding: 0px; border: 0px; outline-style: none; font-weight: inherit; font-size: inherit; font-family: inherit; line-height: inherit; text-align: inherit; vertical-align: baseline;">R-matrix method

Modelling of massive stars and supernovae (SNe) plays a crucial role in understanding galaxies. From this modelling we can derive fundamental constraints on stellar evolution, mass-loss processes, mixing, and the products of nucleosynthesis. Proper account must be taken of all important processes that populate and depopulate the levels (collisional excitation, de-excitation, ionization, recombination, photoionization, bound–bound processes). For the analysis of Type Ia SNe and core collapse SNe (Types Ib, Ic and II) Fe group elements are particularly important. Unfortunately little data is currently available and most noticeably absent are the photoionization cross-sections for the Fe-peaks which have high abundances in SNe. Important interactions for both photoionization and electron-impact excitation are calculated using the relativistic Dirac atomic style="margin: 0px; padding: 0px; border: 0px; outline-style: none; font-size: 14px; font-family: "Lucida Grande", "Lucida Sans Unicode", Tahoma, Verdana, Arial, Helvetica, sans-serif; line-height: inherit; vertical-align: baseline; background-color: rgb(255, 255, 255);">R-matrix codes (DARC) for low-ionization stages of Cobalt. All results are calculated up to photon energies of 45 eV and electron energies up to 20 eV. The wavefunction representation of Co III has been generated using GRASP0 by including the dominant 3d^{style="margin: 0px; padding: 0px; border: 0px; outline-style: none; font-size: 0.85em; font-family: "Lucida Grande", "Lucida Sans Unicode", Tahoma, Verdana, Arial, Helvetica, sans-serif; line-height: 0; background-color: rgb(255, 255, 255);">7}, 3d^{style="margin: 0px; padding: 0px; border: 0px; outline-style: none; font-size: 0.85em; font-family: "Lucida Grande", "Lucida Sans Unicode", Tahoma, Verdana, Arial, Helvetica, sans-serif; line-height: 0; background-color: rgb(255, 255, 255);">6}[4s, 4p], 3p^{style="margin: 0px; padding: 0px; border: 0px; outline-style: none; font-size: 0.85em; font-family: "Lucida Grande", "Lucida Sans Unicode", Tahoma, Verdana, Arial, Helvetica, sans-serif; line-height: 0; background-color: rgb(255, 255, 255);">4}3d^{style="margin: 0px; padding: 0px; border: 0px; outline-style: none; font-size: 0.85em; font-family: "Lucida Grande", "Lucida Sans Unicode", Tahoma, Verdana, Arial, Helvetica, sans-serif; line-height: 0; background-color: rgb(255, 255, 255);">9} and 3p^{style="margin: 0px; padding: 0px; border: 0px; outline-style: none; font-size: 0.85em; font-family: "Lucida Grande", "Lucida Sans Unicode", Tahoma, Verdana, Arial, Helvetica, sans-serif; line-height: 0; background-color: rgb(255, 255, 255);">6}3d^{style="margin: 0px; padding: 0px; border: 0px; outline-style: none; font-size: 0.85em; font-family: "Lucida Grande", "Lucida Sans Unicode", Tahoma, Verdana, Arial, Helvetica, sans-serif; line-height: 0; background-color: rgb(255, 255, 255);">9} configurations, resulting in 292 fine structure levels. Electron-impact collision strengths and Maxwellian averaged effective collision strengths across a wide range of astrophysically relevant temperatures are computed for Co III. In addition, statistically weighted level-resolved ground and metastable photoionization cross-sections are presented for Co II and compared directly with existing work.